R And S 5/4.5 e.
S And SN (NGC 224).
W And S 7.5/1-e.
X And S 5/7-e.
Z And The light curve is characterized
by outbursts up to 4m with intervals of 10 - 20
years. In the intervals cyclic variations are ob-
served with the mean period of 632d and variati-
ons with cycles of several days and delta(m) ~ 0.1m -
0.5m. The spectrum is symbiotic, with features
of a late M giant, narrow low-excitation emission
lines (Bl eq) and forbidden lines characteristic
of highly excited nebulae.
RR And S 6/3.5 e.
RT And Min II 8.88; DI = DII = 0.17P; dI = dII = 0.00. P var.
Nonlinear term: -6.33*10**-11*E**2.
During JD2433477 - 43878
linear elements are satisfactory: Min = 2441141.8888 +
+ 0.62892984d*E.
Period changes
according to a sine law are possible [8002].
RU And P var. Max = 2419857 + 243.0d*E (JD2412800 -
20000); Max = 2434551 + 233.24d*E*(JD2420000 -
34550). Since JD2435000 -
see Table. delta(m) ~ 4m - 5m (before JD2429600),
~ 1m (JD2429600 - 33600), up to 3m (JD -
2436000), ~ 1.5m (JD - 2436700).
In 1970 - 1972
showed quite irregular variations.
RX And SB (P = 0.21173d).
Cyclic variations with P ~ 38s - 54s were obser-
ved after a normal maximum; after a short maxi-
mum no periodicity was found [8004].
SS And Two long period variations are
also observed: P = 650d, P = 3800d.
ST And P var. Max = 2418370 + 337.3d*E (JD2418000 -
28000). Since JD2428000 -
see Table.
SU And VB A (B 12.77m V, F0V:, 15").
SV And The magnitude in Max varies periodically, P = 930d, P =
5400d? [2146].
SW And [Fe/H] = +0.16. P var. Nonlinear term: - 1.229d*10**-10*E**2 [1959]. Since
1959 Max = 2436466.828 + 0.442270121d*E [6929].
The shape of the
light curve varies with Pi ~ 36.83d = 83.28 P. The
deviations (O - C) satisfy the elements of Blazh-
ko effect Max (O - C) = 2436816.23 + 36.921d*N. Se-
cular trend and cyclic (P ~ 2a) variations of
(O - C) are possible [8005].
SY And d = 0.027P.
TT And Min II 11.6?
TU And P var (Pi ~ 37A?).
TV And P var? delta(m) strongly varies.
TW And d = 0.020P. Min II 8.94. P var. Min = 2428845.422 +
4.122739d*E (JD2420050 - 32000). Since
JD2432000 - see Table.
TZ And P1 = 118d: [0882].
Mean magnitude varies with P2 = 974d [0098].
P = 135d (JD2437545 - 38377) [3367].
UU And P var. Min = 2428832.536 + 1.486311d E (JD
2421455 - 23740) [2262]; Min = 2428832.465 +
1.48629D*E (JD2428830 - 35012) [0745].
Since JD2441100 - see Table.
UW And P var. Before JD2430000 Max = 2418585 +
236.7d*E. Since JD2436000 -
see Table.
WW And d = 0.012P.
WX And P var. Max = 2422613.614 + 3.0012544d*E
(JD2422610 - 34712) [1240].
The Table gives current elements.
d = 0.03P in 1972 and probably varies.
WZ And Min II 11.9. P var [2262]. Min = 2435075.342 +
+ 0.695662d*E (before JD2440500);
probably Min = 2440872.290 + 0.6956576d*E
since JD2440500.
The elements in the Table represent all
the observations satisfactorily.
XX And P var. Max = 2418001.938 + 0.7227486d*E (1908 -
1932); Max = 2427106.403 + 0.7227591d*E (1932 -
1946) [2264]. Since 1946 -
see Table. delta(S) = 9. Blazhko effect:
Max = 2437578 + 36d*N [3111].
XY And Blazhko effect is possible.
XZ And Min II 10.16; DII = 0.26P. P var [2431, 6932, 8008,
8593]. Min = 2432883.6046 + 1.3572708d*E (JD
2431700 - 36150) [1977]; Min = 2441954.340 +
+ 1.357293d*E (since JD2436200).
The elements in the Table repre-
sent all the observations satisfactorily.
AA And Min II 10.5.
AB And Min II 10.20. P var.
Period increased sudden-
ly in 1953 ( ~ JD2434500); no period changes
later [2509, 5222]. Elements sin-
ce 1953 - see Table.
AC And Unusual multiperiodical variable.
Second oscillation: Max = 2432467.373 +
+ 0.71124243d*E; P3 = 0.421069d [8187],
see also [8294, 8295]. delta(S) = -1:.
AD And Min II 11.6. Depth
of minima in yellow light: 0.62m (Min I), 0.58m
(Min II) [3141]. Min II - Min I = 0.494P. P var. Min =
= 2428718.402 + 0.9861940d*E (JD2417460 - 29640)
[1983]. Since JD2428700 -
see Table.
AE And In the M31 galaxy.
Strong UV continuum.
Emissions H, He I, Fe II, [Fe II].
AF And See AE And.
AG And According to [8296], DSCT:, Min =
= 2442636.5868 + 0.0347d E, A = 0.5m.
AM And VB A (B 0.25' S).
AN And Min II 6.09.
The existence of the third body in
the system is possible. Sp(Met) = F2 - F5.
AP And Min II 11.9.
The period may be 2 times shorter.
AT And B - V: +0.42, +0.56. delta(S) = 3.
See [8299]
for data on period variations and a detailed stu-
dy.
BD And Min II 11.4.
BE And Average cycle: 137d [1993, 2267];
156.8d after JD2431700.
BL And Depth of Min II 0.24m:. P var? Min I =
= 2429491.255 + 0.7223779d*E (JD2415800 -
33900) [1995]. Since JD2433900 -
see Table.
BX And ADS 1671 A (B 9.7m, 20", 59deg). Min II 9.15.
Possible period change:
from 0.61011222d to 0.61011534d
( ~ 1952).
On the period changes see also [8657].
BY And According to [8658], SRB:.
CC And Possibly in a binary with
Porb = 10.469d. delta(m) and the light curve shape va -
ry with a period 5.23714d or 10.469d [8016]. Accor-
ding to [3120], 4 periods are present: P2 = 0.0632083d.
First overtone was not found. Other periods are
resonances.
CG And P var: 3.7430d (1950), 3.7394d (1963) [5224].
Cyclic period changes are possible.
According to [6941], short period oscillati-
ons (P = 2h 04m) are present. A number of obser-
vers do not find short-term variability.
CM And According to [0821], Max = 2428380 +
+ 140d*E and Max = 2430616 + 124d*E,
and the star resembles UU Her.
CN And Min II 9.96.
CO And d = 0.06P:
CP And d = 0.01P? Depth of Min II 0.05m?
CU And d > 0.034P ([6943],
according to visual observations.
DI And DCEP? [3165].
DK And EW?
DL And In the field
of the open cluster NGC 7686.
DR And P var. Before ~ JD2437000 Max = 2436078.384 +
+ 0.5630609d*E [2275];
then P changed abruptly. delta(m)
changes by ~ 0.3m, Max A1 = 2436078.8 + 69.486d*N1,
Max A2 = 2437646.65 + 69.719d*N2.
Other possible cycles are 2000d (in-
teraction of cycles N1 and N2) and ~ 30 years
[8019].
DS And In the field
of the open cluster NGC 752. Min II 10.7.
DZ And According to
[4008], type RCB, spectrum R. According to [6945],
since 1961 is in Max light all the time. According
to [6946], the spectrum is not characteristic of
RCB stars. According to [8660], The star was
bright near the moments of Min light given in
[4008].
EG And P = 40d or 80d [8020].
Absorption spectrum with overlaying
emissions of high excitation [4434, 8598]. Strong
variable magnetic field [4435]. Long period varia-
tions of light are observed. Radial velocities pro-
files and equivalent widths of lines vary with P =
= 470d [8596] (SB? [8597]). Possibly is analogo-
us to HM Sge [8598].
EH And IR excess. The presence of a dust envelope is possible.
EO And Very red.
EP And Min II 12.5.
ET And delta(B) = 0.035m, delta(U) = 0.07m.
The Table gives the epoch of Max
light. Observations may be represented by the pe-
riods 0.723d and 1.61553d [8022, 7946]. According
to [8023], in June - December 1977 Min =
= 2443337.4725 + 0.49925d*E, other periods are
not satisfied by observations. According to [8599],
Max(U) = 2439751.28 + 0.617135d*E (1967 - 1971).
SB, Max(Vr) = JD2443718.0 + 48.304d*E [8301].
Photometric periods could not be found in radi-
al velocities.
EX And Possible Min II 13, 0:, Min II - Min I =
= 0.55P.
EY And I - K = 5.38;
The presence of a dust envelope is possible
[6947].
FF And 10.35m - 10.42m V outside flares;
M - m = 0.50P. Porb = 2.170304d [8024].
According to photomet-
ric observations P = 2.14d (1971), P = 2.15d (1972),
P = 2.19d (1973) [6948].
FG And According to [4156], EA; Min =
= 2436074.528 + 0.99772d*E.
FL And d = 0.02P.
FZ And mu = 1", p = 64deg.
GK And Min II 11.5.
GN And ADS 409 A (B 13.3m, 2", 6deg; C 11.6m, 141", 130deg).
Different
authors give spectral types F0 III, F2V, Am (pro-
bably based on different criteria).
GP And delta(m) changes with P2 = 0.64d.
A wave with P3 = 0.012161d is present. The mean
magnitude and the shape of the light curve vary
[8302].
GQ And ADS 246 B (A = GX And; B 37", 61deg). B - V = +1.80.
X-ray source.
GR And Min (magnet.field) = 2442288 + 525d*E.
Magnetic field varies ( - 250
to - 1030 Gauss). Period of changes of C1 is near
1.5 years [7893]. According to [6257], period
of changes in u is near 1 year or longer.
GS And B - V = +1.7 in normal light.
GX And ADS 246 A (B = GQ And, 37", 61deg). delta(U) = 0.55m. SB?
(conflicting data).
GY And SB 1 (P = 273.2d [7324], P = 272.99d [8303]).
For spectral changes, variations of
light and magnetic field it is possible that P =
= 23a [7004] or 20.60a [8303]. [8022] gives P ~ 36.5d
and delta(V) ~ 0.049m. Periods 4.92a and 1.8d may exist
[8303].
GZ And B - V: +0.77, +0.82. ADS 1693 A (B 11.13m, 8", 31deg).
Min II 11.58. P var.?
The period is based only on Minima I [6830] and
was improved with account of recent data.
HH And Subdwarf? [6581]. mu = 1.82", P = 176deg.
HI And B - V = 1.8m outside flares.
HN And Max(U) = 2438327.8 + 69.433d*E [8022]. SB
(P = 106.27d [7435]).
HQ And According to [8659], a probably
cataclysmic binary; similarity to AM Her and AN
UMa is noted.
HR And d = 0.05P.
HT And B - V = +0.60. In the region of M 31.
HU And Min II 17.2. In the region of M 31.
HV And See HQ And.
HY And In the region of M 31.
HZ And See HY And. P > 100d. Red.
IL And d = 0.02P.
IM And See HY And. Min II 18.8.
IO And See HQ And.
IP And d = 0.02P:.
KK And The light curve has double-wave shape
[7740]. Long period variations were found [7955].
KU And I - K = 4.63.
SR type is possible. Surrounded with a dust envelope [8029].
KX And SB 2 (P = 38.908d).
KZ And ADS 16557 B (A 7.0m; B 15", 254).
LM And Min II 12.7.
LN And delta(B) = 0.025.
LO And Min II 11.82.
alf And SB (P = 96.6960d). VB A (B 11.2m, 80").
Epoch of Max U light is given.
H beta index varies in the range of ~ 0.02m with P
~ 3h [8030]. Rapid rotation.
zet And Depth of Min II 0.1m. SB.
Unstable light curve. Most notable
variations on the rising branch of Max II [8030].
Many peculiarities in the spectrum.
lam And SB 1 (P = 20.52d).
omi And V sin I = 300 km/s; VB(0.3"; possibly
also 0.05" -
according to speckle-interferometric data).
Shell spectrum appeared and disappeared seve-
ral times since 1890. Different authors attributed
the star to EB type. According to [5955], The chan-
ges of light may be explained also by intrinsic
variations of a single shell star. They are repre-
sented by elements: Min I = 2439470.628 + 1.0185d*E.
according to [2572], Min I = 2436174.430 +
+ 1.5998398d*E. The periodogram analysis shows
a stable peak at P ~ 0.84P [8032]. A possible shell
event was observed late in 1975.
S Ant Min II 6.87. P var?
T Ant CWB? P var. [A/H] = -0.0. P = 5.9098d (JD2428187 -
34688), P = 5.8976d (JD2434688 - 37660) [5387].
The Table gives mean elements which satisfy
all observations well enough.
V Ant OH, H2O maser.
Z Ant Mean brightness va-
ries with P = 1143d.
SW Ant Min II 14.6.
UZ Ant P var?
WY Ant P var. P = 0.57430871d (JD2414000 - 22070); P =
= 0.57431618d (JD2422070 - 25600); P = 0.57431216d
(JD2425600 - 29000) [1113]. (k - b)2 = 0.00.
WZ Ant Min II 11.8.
XX Ant Min II 9.1.
XY Ant Depth of Min II 0.3m - 0.5m pg.
XZ Ant Min II 10.2.
Z Aps Possibly
also an eclipsing binary.
RT Aps Strong variations of period and the shape of
the light curve [6152].
TY Aps delta(S) = 3.
YY Aps The period is pro-
bably long.
AF Aps Min II 13.9.
AN Aps Min II 12.8.
AP Aps Min II 15.5.
AS Aps Min II 13.8.
AV Aps Depth of Min II 0.05m.
CE Aps P = 209d or 261d.
CY Aps Min II 13.0.
EF Aps Min II 12.6.
FY Aps Deep Min II.
GK Aps Min II 13.9. RRC type is possible.
GO Aps Min II 14.8. RR type is possible.
GQ Aps Min II 14.8.
GU Aps Min II 14.5.
GX Aps RV type
is not excluded. The epoch of Min is given.
GY Aps Min II 14.2.
HL Aps Min II 12.6.
HO Aps Min II 13.7.
HT Aps Min II 14.3.
HV Aps Epoch of Min is given.
HX Aps Min II 14.4.
II Aps Min II 11.6.
IL Aps See HV Aps.
IO Aps Min II 12.4.
IR Aps Min II 13.8.
IU Aps Min II 14.6.
IY Aps Min II 12.9.
KN Aps d ~ 0.03P.
KR Aps Possibly a
slow eclipsing variable.
KT Aps Min II 15.2.
KV Aps Min II 13.6.
KZ Aps Smooth light
changes with superimposed variations of eclip-
sing nature, with minima on JD2436729 and
2436808.
LM Aps RV type is possible.
LN Aps Min II 13.3.
LO Aps Min II 11.5.
MY Aps L19 - 2. P0 = 192.75s, P1 = 113.77s.
del 1 Aps In a wide pair (delta**2 Aps, 100",
common mu).
kap 1 Aps SB? VB A (B 11.27m V, 27").
R Aqr Symbiotic spectrum. Emissions
of H, SII, OIII, FeII, NeIII, OII. Variable radio sour -
ce. SiO maser. The secondary may be an accre-
ting white dwarf. The star is embedded in an ex-
panding gaseous nebula several hundred years
old. A cycle ~ 24a and longer-term variations are
possible in the changes of radial velocities and
period.
U Aqr Strong bands of 12C2, CN,
lines of SrII, YII in the spectrum; hydrogen defici-
ency. A probable halo star (Vr ~ 100 km/s.).
Z Aqr 1969 - 70: P = 100d +- [5973].
RY Aqr P var. Min = 2433872.352 + 1.966598d*E (before
JD2428000); Min = 2440824.410 + 1.966620d*E
(JD2428000 - 41000); Min = 2440824.410 +
+ 1.966611d*E (JD2441000 - 43800). Since
JD2443800 P = 1.966554d?
The Table gives elements represen-
ting observations after JD2428000 with the accu-
racy +- 0.1d.
ST Aqr Min II 9.37. P var. Min = 2423640.271 + 0.78101367d*E
(JD2423500 - 26000) [2037]. Since
JD2439700 - see Table.
SU Aqr ADS 16318 A (B 10.7m, 5", 144deg). Min II 10.5. P var?
SV Aqr Cycle 200 - 300d is possible.
SW Aqr P var. (k - b)2 = 0.01.
SX Aqr P var? delta(S) = 9.
SZ Aqr Epoch of Min is given.
TT Aqr VB A (B 15m, 3", 135deg).
TZ Aqr delta(S) = 5.
VY Aqr Second outburst: Max ~ JD2437897
(1962), ~ 9m pg [3129].
WX Aqr Blazhko effect is pos-
sible.
XZ Aqr P var. Before JD2437913 P = 2.059187d.
YZ Aqr B - V = 0.49 (in Min). (k - b)2 = 0.06.
Small fluctuations
of period are possible.
AE Aqr Unusual
flare X-ray system with pulsar. Becomes bluer
in Max. In Min B - V = +0.92. Shows rapid irregular
variations, which differs it from UV stars and UG
system, though the spectra are somewhat similar.
Simultaneous photoelectric and spectroscopic ob-
servations [3131] show the existence of two types
of flares: 1) intensification of emission lines ac-
companied by brightening in U and B; 2) intensifi-
cation of continuum leading to brightening in U,
B and V ("white flare"). Detailed spectroscopic
investigation [1971]. Porb = 0.41165794d +
+ 1.12*10**-10*E, The epoch T0 = JD2439030.621
[8672]. In the X-ray band (0.1 - 4.0 keV) pulsati-
ons with P = 33.0767s are observed [8673]. In the
optical range pulsations with P0 = 33.076737s as
well as with P1 = 16.5s were noted [8674, 8675].
AT Aqr Min II 14.7.
AX Aqr P var. Before ~ JD2427367 Max =
= 2425417.60 + 0.388135d*E [3113].
AY Aqr Min II 14.3.
BH Aqr P var. Before ~ JD2431150 Max = 2426948.411 +
+ 0.5258022D*E [3113].
BI Aqr Min II 13.1.
BK Aqr Close companion.
BL Aqr Waves from 80 to 125d. Mean magnitude changes
with cycles from 480 to 700d in the range of 0.3m -
0.6m.
BM Aqr The mean magnitude may vary with
P = 500 - 600d.
BN Aqr delta(S) = 4:. P var. Before JD2428964 Max =
= 2426577.901 + 0.46963401d*E [3113].
According to [5391] Max = 2429395.742 +
+ 0.4696410d*E + 3.3*10**-10*E**2 (1898 - 1958).
BO Aqr P var? (k - b)2 = 0.01.
BQ Aqr d = 0.07P.
BR Aqr P var? (k - b)2 = 0.16.
BS Aqr delta(S) = 0. P var?
BT Aqr B - V: +0.14, +0.52. P var.
Blazhko effect.
BV Aqr P var.
Blazhko effect with Pi =
= 11.56d and variations of light in Max up to 0.75A.
BW Aqr d = 0.01P. Min II 10.8. Min II - Min I = 0.484P.
Jensch [0189] considers the secondary Min to be the
main one.
BX Aqr d = 0.027P.
CD Aqr d = 0.012P. Min II 10.2.
CE Aqr According to [2548], no
variations were found in visual observations du-
ring several months in 1954 - 1958. According to
[3138], The star may be analogous to AI Vel; P =
= 0.16d?
CH Aqr P var?
CI Aqr Period may
be twice as long.
CM Aqr Min II 13.6.
CP Aqr delta(S) = 3.
CR Aqr Min II 14.2.
CV Aqr Data in [6072] are not reliable.
CW Aqr Min II 10.8.
CX Aqr Min II 10.8. Broad hydrogen lines.
CY Aqr delta(S) = 2. P var; abrupt
change ~ 1952. Before JD2434000 Max =
= 2434308.4314 + 0.061038509d*E. The shape of
the light curve probably varies. For M - m diffe-
rent authors give values from 0.23p to 0.40p. Beat
phenomenon with P2 = 0.2182d is possible [8060].
CZ Aqr Min II 11.1. Cyclic variations of period?
DD Aqr Min II 11.2.
DN Aqr (k - b)2 = 0.01.
DO Aqr P var.
DS Aqr P var.
DV Aqr Min II 6.1. SB.
In [8061] variations were noted
with delta(m) ~ 0.1m and P < 3h, presumably of DSCT
type nature. Some sources give A3 for the spect-
ral type. Shell spectrum was observed in May,
1975. Spectral lines were filled with emission
and therefore weak, strong absorption in H and
K CaII lines was present. Shell effects were not
present in the spectra taken in 1971 - 1973 [8062].
DX Aqr VB B (A 7.0m, K0 III; B 3.7", 244deg). SB 1. d ~ 0.015P.
Depth of Min II ~ 0.3m.
The range of combined brightness is given.
DY Aqr d = 0.04P.
EE Aqr Min II 8.48.
EK Aqr Min II 11.23.
EL Aqr P = 0.6345d is possible.
EM Aqr According to [6204] P = 0.068d.
Period and amplitude vary on very short time
scale. Light and colour vary approximately in pha-
se. The beat period, if exists, is shorter than 1d.
ET Aqr Period is given according to [8336].
EW Aqr delta(m) varies.
FF Aqr d = 0.059P. SB 1.
The unique eclipsing system of a
red star and probably a blue hot subdwarf. The am-
plitude of the eclipse is 0.15V, 0.4B, 1.2U. The
magnitude in Max varies by 0.35V, 0.33B, 0.22U.
variable shape of light curve. Strong emissions H
and K CaII, H alfa in the spectrum.
FI Aqr Possibly P = 4.659d or 4.719d.
Epoch of min is given.
FK Aqr BDS 11854 A(B = FL Aqr, 11.45m, 24", 352deg, 1966).
mu alfa = +0.455", mu delta = -0.067". SB 2 (P = 4.08322d [0313])
Flares delta(U) = 0.7 [0344].
FL Aqr BDS 11854 B (A = FK Aqr; B 24", 352deg, 1966).
omi Aqr Shell
or disk spectrum is observed.
pi Aqr The brightness increased by ~ 0.2m V
in 1957 - 1975, the star became redder. Balmer
continuum in emission. Rapid changes in emissi-
on lines and in polarization. Existence of a disk
or a shell is possible.
R Aql P var. Max = 2440038 + 297d. E (JD2427850 - 40000).
Since JD2440000 - see Table.
For the whole obser-
ved period Max = 2399190 + 346.932d*n - 0.239303d*n**2;
Pn = 348.980d - 0.554202d*n + 0.000552309d*n**2 [3143].
H2O, OH and SiO maser. Radiobursts.
U Aql B - V: +0.84, +1.24. P var. ADS 12503 A (B 14.00m,
35", 349deg, 1900; one more compa-
nion 11.7m V, 2", 230deg, 1934).
W Aql S 6/6e.
Composite spectrum near Min light; a companion
(F5 - F8) may exist [3502].
Y Aql Depth of Min II 0.03m. SB 1.
RR Aql Maser H2O, OH, SiO.
RT Aql See RR Aql.
SY Aql Maser H2O, OH.
SZ Aql B - V: +1.04, +1.82. P var [2392]. Before
JD2420260 P = 17.1359d.
Current elements - see Table.
TT Aql B - V: +0.96, +1.62. P var. [2392]. Before
JD2418035 P = 13.7518d.
Current elements - see Table.
TV Aql P var (changed at ~ JD2430000).
Before JD2430000 Max = 2429730 + 237.9d*E.
TW Aql Cycles 65d or 95d are
observed during different time intervals [8714].
UU Aql Mean cycle: 71.3d [4063]; 56d
[3144].
UY Aql Cyclic changes of
light (P ~ 400d) with superimposed very rapid va-
riations are noted in [0504].
VX Aql SC 5 - /8e.
According to [4231], the varia-
ble is irregular. Lithium star.
VZ Aql B - V: +0.61, +1.01.
XZ Aql P var. Min = 2424449.277 + 2.139147d*E
(JD2424380 - 2430300). Since
JD2433000 - see Table.
YZ Aql d = 0.03P. P var.
AA Aql delta(S) = 1.0.
AC Aql P var.
AD Aql CN bands are
observed in the spectrum. According to [6928],
The range is 8.83 - 13.42 V.
AE Aql VB A (B 16.6m, 12", 330deg; C 16.9m, 11", 0deg).
The combined light of A, B, C varies in the ran-
ge 13.9 - 15.8.
AF Aql The period
may be two times shorter.
AL Aql d = 0.04P.
AU Aql According to [3146], P = 190d or
380d.
BL Aql P var. Max = 2418538 + 159.65d*E (JD2418529 -
- 29075). During JD2436420 -
- 38940 - see Table.
BY Aql P var?
CD Aql Close companion?
CL Aql Sometimes maxima predicted according to the
elements do not occur.
CM Aql Symbiotic spectrum similar to
that of Z And [3149].
CR Aql Considerable Blazhko effect is possible.
CS Aql See CD Aql.
CT Aql According to [6004], only slow
irregular variations with delta(m) ~ 0.6 were observed
in 1963 - 1968.
CU Aql P var? (Possible change
~ JD2423000). Earlier Max = 2418591 +
+ 203.7d*E.
CV Aql P var?
CW Aql See CD Aql.
DD Aql See CD Aql.
DT Aql P var (Change ~ JD2425000).
Earlier Max = 2423964 + 290.5d*E.
DY Aql P var [6107].
EV Aql P var. Before JD2423900 P = 38.67d.
[A/H] = -0.3.
EX Aql P = 117d is also
observed.
EZ Aql P var [6107].
FF Aql ADS 11884 A (B 10.37m, 7", 141deg). SB 1 (P = 1435d).
FG Aql At the edge
of the dark nebula Barnard 130. May be a physi-
cal pair with FH Aql (ro ~ 20"). According to
[0504], The mean cycle of light variations is 3.5d.
The level of mean light varies.
FH Aql On the position and binarity See FG Aql.
According to [0504], the mean cycle of light va-
riations is 3.44d.
FK Aql Dept of Min II 0.03m. P var.
FM Aql B - V: +1.12, +1.50.
FN Aql B - V: +1.10, +1.39. P var.
FZ Aql VB A (B 11.5m, 14", 162deg).
GM Aql UV type is possible [0504].
GU Aql d = 0.02P.
GV Aql Nova-like star according to [2089].
GY Aql Maser OH, SiO.
HK Aql Type ISB is not excluded.
HL Aql P var?
The 15m star shown in the charts
[2274, 6996] with co-ordinates coincident with
those given at the discovery is constant accor-
ding to [2274].
IM Aql P var. Before JD2432772 Max = 2428064.707 +
+ 0.4569602d*E.
IO Aql VB A (B = IP Aql, 30", 101deg).
IP Aql See IO Aql.
IS Aql Close companion.
KL Aql B - V: +0, 78, +1.19, [A/H] = 0.6.
KO Aql d = 0.018P. Min II 8.40. P var. Min = 2427550.565 +
+ 2.863859d*E (JD2426250 - 33000) [2462]; Min =
= 2433888.366 + 2.863954d*E (JD2433000 - 39000).
Current elements - see Table.
KP Aql Min II 10.43; Min II - Min I = 0.50P; DII = DI.
KV Aql During JD2429130 - 31370 - see Table.
During JD2428308 -
- 28433 the star was faint. Max 2436015 also is
not satisfied by the elements.
LU Aql In [3158] P = 102D is given, and the exis-
tence of the variation of mean magnitude with P ~
~ 1080d and delta(m) = 0.4m was suspected.
MV Aql Close component, the range is
given for combined light.
NN Aql Cyclic P variations?
NV Aql Variations of mean light with P ~ 900d -
- 1000d and delta(m) ~ 0.6m.
OO Aql Min II 9.8. P var. Min I = 2426892.0582 +
+ 0.5067954d*E (1932 - 1934), Min I = 2433925.3762 +
+ 0.5067943d*E [8072]. Since JD2438000 -
see Table.
The shape of the light curve varies.
OX Aql Var 2 in the chart for OW Aql.
PP Aql [A/H] = -0.0. CWA type
is not excluded. According to [3161]
P var. Max = 2415229.15 + 24.0147d*E (JD2415228 -
- 21064), Max = 2426576.14 + 24.074d*E (JD2426576 -
- 29489). After JD2432040 Max =
= 2433141.78 + 23.994d*E.
Current elements Max = 2436836.04 + 23.973d*E.
PZ Aql P var? According to [5387], before
JD2428075 P = 8.7555d; P = 8.7504d
(JD2428075 - 34725); since JD2434725
P = 8.7573d. See also [2274].
Elements in the Table are satisfactory after JD2433150.
the shape of the light curve apparently varies.
QS Aql Min II 5.97. VB (A 6.5m; B 6.7m, 0.18", 137deg).
P var.
QV Aql The epoch of main Max is given.
QY Aql d = 0.016P. P var?
V 336 Aql B - V: +1.17, +1.55.
V 337 Aql Min II 9.09. P var.
The shape of the light curve varies.
V 340 Aql d = 0.05P. P var.
V 341 Aql P var. delta(S) = 4.
V 342 Aql ADS 12259 B (A 7.5m; B 20", 14deg); d = 0.032P. P
increases (See also [2265, 4493]). Before JD2435600 Min =
= 2428023.550 + 3.390842d*E.
H alfa emission observed at Max light [8074]. The shape
of the light curve and dapparently vary. delta(m)
probably decreases [8075].
V 343 Aql Min II 10.7.
V 346 Aql Min II 9.1. ADS 13438 A (B 11.3m, 2", 245deg).
Elements in the Table are valid after
JD2437000. The shape of Min I varies [7001].
V 348 Aql d ~ 0.08P.
V 352 Aql The nucleus of the supposed planetary nebula P.K.
37 -3.3deg.
V 356 Aql VB A (B 0.2").
V 367 Aql The elements are satisfactory
only during JD2436450 - 37960. Resembles
S Vul (SRD).
V 368 Aql VB A (B 0.17", 140deg).
V 374 Aql VB A (B ~ 0.2', ~ 270deg).
V 406 Aql Min II 13.3:.
V 407 Aql P var;
There is nonlinear term in the elements:
+ 1.51d*10**-9*E**2.
V 409 Aql Min II 12.2.
Spectral type from another publication
is A2 - A3.
V 411 Aql Epoch of Min is given.
V 417 Aql Min II 11.5. P var. Before JD2439000:
Min = 2428427.127 + 0.3701251d*E.
V 421 Aql P var?
V 423 Aql Elements are valid
for JD2426900 - 28000. During
JD2429020 - 31670
The waves are much lon-
ger or absent.
V 433 Aql Waves of 26d - 80d durati-
on with delta(m) = 0.1m - 0.9m. The mean light varies
according to the formula Max = 2438312 +
+ 648d*E.
V 461 Aql Close component ~ 15.5m, the
range of combined light is given.
V 467 Aql Waves of 40d - 72d duration. The
mean light varies with P ~ 1400d.
V 473 Aql P ~ 330d is so-
metimes observed.
V 476 Aql EW type with doubled period is
possible. Elements are based on a short series
of observations.
V 483 Aql In the field of the open cluster NGC 6709.
V 486 Aql See V 483 Aql.
V 493 Aql B - V: +1.10, +1.38.
V 495 Aql d = 0.06P:.
V 496 Aql B - V: +1.07, +1.28.
Elements are given for
epochs after JD2428000.
V 497 Aql VB A (B 16.5m, 9", -0deg).
V 524 Aql The variable is np from the
star shown in the chart in [2317].
V 527 Aql IS type is possible.
V 528 Aql VB A (B 16.5m, 11", 59deg).
V 535 Aql VB.
[1943], Two components are seen
on palomar prints, eastern of them being red.
according to [1943], rapid variable.
V 537 Aql Possible P = 200d.
V 538 Aql Possible P = 375d.
V 558 Aql Possible P = 187d.
V 571 Aql Possible P = 185.5d.
V 572 Aql B - V: +0.65, +0.87. P var. Before
JD2435500 P ~ 3.7686d. See also
[8637].
V 586 Aql Irregulari-
ties are sometimes observed, but then the pe -
riodicity is probably resumed.
V 596 Aql Resembles S Vul.
V 599 Aql Min II 6.73.
According to [8083], may be constant.
V 600 Aql B - V: +1.36, +1.70.
Before JD2428000
another value of P is possible [8632].
V 602 Aql d = 0.02P. Min II 12.7.
V 603 Aql SB (P = 0.13854d [3169]).
Outside the outburst there are varia -
tions of light (eclipses) with delta(m) = 0.30m,
Min I = 2444401.399 + 0.1377d*E (D ~ 0.2P). The
shape of the light curve and the depth of mi -
nima differ from cycle to cycle. The bright-
ness in minima shows fluctuations apparent-
ly connected with the presence of a hot spot
[4500].
V 605 Aql A unigue
variable. 8" np from a 17m star. Min ~ 20m pg.
photographs of the field [6041, 6042]. The
light curve resembles those of the SN in NGC
1058 or of eta Car [6040]. The only Max obser -
ved, with fluctuations, occured in 1918 - 1924.
In 1921 the spectral type was found to be R
[2464]. The star is inside the old planetary ne-
bula A 58 and may be its nucleus.
V 609 Aql Min II 11.9.
V 615 Aql P var? Max = 2428046 + 364d*E (JD2428038 -
- 31343) [1091].
V 616 Aql d = 0.04P. Ele-
ments reguire verification.
V 618 Aql Twice
shorter period is not excluded.
V 637 Aql See V 618 Aql.
V 638 Aql See V 618 Aql.
V 640 Aql Min II 12.8.
V 647 Aql Slight Min II [1091].
V 663 Aql P = 194.5d is possible.
V 666 Aql The range is given for combined ma-
gnitude with a preceding 16.5m star. Separately
was found ~ 17m pg near Min.
V 672 Aql P var? Blazhko ef-
fect is possible [3113].
V 678 Aql P var. Before JD2429723 Max = 2429723 +
+ 120.6d*E.
V 688 Aql Min II 10.8. DII = 0.15P.
V 694 Aql d = 0.13P. VB (1"),
a companion ~ 1m fainter than
the variable [1881] may have affected the data
given.
V 699 Aql Min II 13.75.
V 706 Aql delta(S) = 0:.
V 708 Aql P ~ 65d waves superimposed on slow variation
of mean brightness with P ~ 1350d (JD2437124 -
- 40512) [6025]. According to [0773] waves
with P ~ 100d - 150d (JD2427543 - 31318).
V 714 Aql d = 0.05P.
V 724 Aql Min II 11.57.
V 733 Aql P var? Before JD2434500,
possibly Max = 2434453.72 + 6.17687d*E [0001].
V 734 Aql VB A? (B 16.1m?).
V 743 Aql White. SRD?
V 755 Aql Alternative elements: Min = 2429195.290 +
+ 1.01598d*E.
V 765 Aql B - V: +0.70, +0.80.
V 766 Aql EW type is not excluded.
V 769 Aql d = 0.05P?
V 770 Aql Min II 14.0.
V 771 Aql According to [3165] UG.
V 774 Aql Possibly resem-
bles UV Boo.
V 777 Aql P = 111.5d is possible.
V 784 Aql Min II 14.8.
V 794 Aql Rapid changes with delta(m) up to
1.5m superimposed on slow ones. May belong to
"polars" of XPRM type. Peculiar spectrum
with broad emissions and blue continuum [8676].
V 800 Aql VB. According to [6072] UGZ.
V 801 Aql VB A (B 15.1m sp).
V 803 Aql Min II 14.8.
V 804 Aql Min II 12.8. In Max B - V = +0.61.
V 805 Aql Min II 7.90, DII = 0.11P.
V 808 Aql Min II 13.3.
V 812 Aql VB A (B 16m sp, C 16m sf).
V 814 Aql VB A (B 16.5m sp).
V 822 Aql Min II 7.07. ADS 12538 A (B 10.1m, 1", 67deg).
The shape of the light curve varies.
(U - B) index in Min I is redder and Min II is
bluer than average.
V 829 Aql Twice
longer P is possible.
V 836 Aql RR type is possible
([0085]; it is suggested also by the spectrum
[8676]).
V 850 Aql In the cent-
re of the planetary nebula P.K. 37 -6.2.
V 866 Aql Min II 14.8.
According to [6026], the depth
of Min II 0.4m, EB type.
V 867 Aql P var?
V 871 Aql Min II 14.5, Min II - Min I = 0.425P.
Physical changes in the range 13.3 - 13.6 are
possible. Eclipses start from the 13.6m level.
V 872 Aql Min II 15.7:.
Apsidal motion is possible.
V 873 Aql P var?
The mean light varies in the range
13.8 - 14.0.
V 875 Aql White. According to [6004], ra -
pid. Possibly UGZ or IA.
V 877 Aql VB A (B 16.5m nf).
V 882 Aql Blazhko effect is
possible.
V 885 Aql Min II 14.9:.
Apsidal
motion and changes of the shape of the light
curve are possible.
V 888 Aql A possible member of the open clus-
ter NGC 6738.
V 889 Aql Min II 9.0. Min II - Min I = 0.35P.
Apsidal motion is possib-
le.
V 890 Aql Nova Aql 1946 = asteroid N258 Tyche
[9038].
V 891 Aql Min II 15.8.
V 895 Aql P var. Max = 2430931.435 + 0.265108d*E
(JD2426920 - 35010) [2267].
During JD2441890 - 42290 - see
Table.
V 907 Aql Min II 15.7.
V 912 Aql The shape of
the light curve varies.
V 914 Aql P = 3.336217d
is given in [8717] by misprint.
V 919 Aql Min II 13.8.
V 920 Aql F or earlier ob -
servations Max = 2429458.400 + 0.4955033d*E.
V 922 Aql Elements are
not quite reliable.
V 923 Aql Unusual shell star [1884]. Similar to EW Lac.
He lines are widened by the rotation, NaI lines
are narrow. Light changes are periodic: Min =
= 2436458.66 + 0.8518d*E. The cause of varia -
tions is probably connected with the rotation
and the inhomogeneous brightness distribution
over the disk of the star [3178]. Profiles of
spectral lines vary. The expansion of the enve -
lope terminated in 1965, which apparently led
to the development of inhomogeneities and to
the broadening of hydrogen line profiles [4525].
V 925 Aql Some observers found cons -
tant brightness [3165].
V 929 Aql Short period.
V 936 Aql See V 929 Aql.
V 947 Aql According to [5412], rapid irregular
changes are not excluded. According to [0504],
constant.
V 955 Aql Min II 14.9, DII = 0.13P.
V 956 Aql Min II 14.2.
Elements need confirmation.
V 957 Aql P var. Max = 2428154.960 + 0.6051327d*E
(JD 2421871 - 28105).
V 958 Aql VB A (B 17.0m, 0.2' np; C -
slightly brighter, 0.1'f).
Combined magnitude of A
and C is given.
V 964 Aql Min II 13.7.
V 969 Aql Blazhko effect is
possible.
V 981 Aql Min II 14.5.
V 991 Aql IS type is possible.
V 992 Aql According to [4260],
P = 110d.
V 998 Aql The position coincides with the pla-
netary nebula P.K.50 - 3.1deg.
V 999 Aql Tsessevich's
observations [7806] do not agree with the ele-
ments in the Table.
V 1017 Aql Elements
need confirmation.
V 1033 Aql P var?
V 1045 Aql Min II 13.5.
V 1046 Aql P var? [8321].Min = 2427713.314 + 5.28303d*E
[4027].
Slight reflection effect is possible.
V 1064 Aql Cycles 295d - 410d.
V 1072 Aql sp component
of a close pair.
V 1075 Aql d = 0.04P. Min II 13.6.
V 1076 Aql VB A (close preceding).
V 1086 Aql VB.
Probably the variable is the sf component.
V 1093 Aql IA type is possible.
V 1095 Aql P var. After JD2429048 -
see Table, earlier Max = 2427322 +
+ 42.68d*E. Not coloured appreciably.
V 1096 Aql Min II 13.3.
V 1097 Aql Min II 14.0.
V 1101 Aql Possibly UGZ
type [3156].
V 1113 Aql The period may be twice shorter.
V 1117 Aql Min II 16.6.
V 1125 Aql Min II 16.0.
V 1140 Aql P var?
V 1154 Aql Min II 14.8; Min II - Min I = 0.70P.
V 1165 Aql According to [4564], constant. In [3932]
was not separated from a close component
which probably led to distortions of the light
curve.
V 1166 Aql UG type is possible.
V 1173 Aql nf component of
a close pair.
V 1182 Aql Min II 8.65.
V 1184 Aql Min II 13.4.
V 1200 Aql VB.
The variable is the eastern red com -
ponent.
V 12O4 Aql VB. The
variable is the eastern component.
V 12O8 Aql A common prorer motion star
9.06m in 1' to the south.
V 1248 Aql UG type is possible.
V 1251 Aql Red.
V 1261 Aql Spectral type K2 in HD.
V 1269 Aql VB. The
variable is the preceding component.
V 1281 Aql Reddish.
SRD type is possible.
V 1286 Aql Possibly the
period is accidental.
V 1288 Aql ADS 12182 A (B 12.3m, 36", 287deg).
V 1291 Aql The elements
have been determined on the base of magne -
tic field variations. The epoch of minimum
intensity of the magnetic field is given.
V 1295 Aql Shell star. Dramatic
spectral changes were observed [5240].
The variability is hardly periodic, though
P ~ 100d is possible. Sometimes light fluctua -
tions on several days' time scale are obser -
ved [5880]. IR excess [6277]. For a detaliled
spectroscoric study, with evidence for the
outflow of matter from the surface, see [4739].
Considerable magnetic field [4435].
V 1297 Aql d = 0.05P? Min II 14.5.
V 1298 Aql mu alfa = -0.0392s, mu delta = -1".330.
The companion of the star BD +4deg 4048 (ro =
= 73".8, teta = 151deg 5).
One of the absolutely faintest known stars
(Mv = +19m).
V 1300 Aql I - K: +5.2, +6.5.
Sometimes maser emission CO, SiO, OH.
V 1302 Aql A unique IR object
IRC +10420. B - V = +2.7, U - B = +1.9. OH - ,
H2O - , SiO - maser.
According to [7437], The
energy distribution in the IR spectrum (1 - 22mkm)
resembles that of eta Car. Emissions of neut-
ral metals are observed in the spectrum. Incre-
ased in brightness during 1925 - 1970; Max ~ 1970.
V 1323 Aql Close VB; var -
northern component.
V 1331 Aql Min II 7.95. According to [4619]
P = 1.364076d.
V 1333 Aql Aql X - 1.
Light variati-
ons with P ~ 1.28d - 1.31d due to orbital moti -
on are possible [4625]. Bursts characteris-
tic of the XB type are observed [4757]. Lx/
Lopt ~ 500 outside nova-like bursts, Lx/Lopt
~ 5000 during bursts.
V 1336 Aql In 1.6' W from MXB 1916 - 05.
M type is possible.
V 1340 Aql d = 0.06P?
Intrinsic light variations in
Max are possible.
V 1341 Aql Min II 13.4. P = 0.3586768D is po -
ssible.
V 1343 Aql SS 433. = +2.0.
Associated with the SNR W 50. Mean light va-
ries in the range 14.0 - 14.6 V according to the
elements Max = 2443662.5 + 165.5d*E [0512].
The depth of Min I varies from 0.2m to 0.9m V,
the depth of Min II varies from 0 to 0.4m V. Two
systems of H, HeI, HeII emission lines are ob -
served in the spectrum: the "stationary" sys -
tem corresponding to Vr changes from 300 to
150 km/s with P = 13.1d, and the "relativistic"
one, corresponding to Vr changes from +50000
to - 35000 km/s with P = 165.5d. The spectral
study [0535]. The system apparently consists
of an O - B star filling its inner roche lobe
and a compact object surrounded by an accre-
tion disc wich is precessing with P = 165.5d.
Two jets consisting of dense condensations of
matter emerge from the system with relativistic
velocity (0.27 c) in opposite directions. The
luminosity of the disc amounts to not less
than 60% of the total luminosity of the system
[0926, 0953]. The object may be a former su -
pernova which bursted not more than 10**4
years ago.
V 1345 Aql Min II 14.3:, Min II - Min I = 0.46P.
V 1349 Aql Max ~ 17 pg.
V 1352 Aql VB A (B 14.5m, 6", 175deg).
V 1353 Aql Min II 10.9.
V 1355 Aql Min II 13.3.
V 1357 Aql Possibly P = 1.051d.
eta Aql P var. P = 7.176344d (JD 2373000 - 95100),
P = 7.176455D (JD 2395100 - 2412100).
Since JD 2412100 - See Table.
for the
whole interval Max = 2442794.773 + 7.176735d*E +
+ 2.18d*10**-8*E**2 [8632].
In the UV band the light of a
possible A0V comparion is apparent.
sig Aql ADS 12737 A (B 12.34m, 48", 328deg).
Depth of Min II 0.1m.
In
[4627] P = 1.950271d is given according to
spectroscoric data.
R Ara Min II 6.2. VB A (B 8.2mV, 4", 123deg).
S Ara (k - b)2 = 0.09. P var [1932, 3126]. Max = 2416284.792 +
+ 0.45188910d*E (JD 2414000 - 19000);Max =
= 2419149.797 + 0.45188581d*E (JD 2419000 -
- 30000) [0752]. Since JD 2441000 -
see Table.
For the whole interval, with suf-
ficient accuracy, Max = 2420047.2382 +
+ 0.451888176d*E - 1.36d*10**-10*E**2 [3126].
T Ara VB A (B 11.0m, 34", 60deg).
X Ara Shown in the
chart for S 5809.
RT Ara According to
Cannon [1944] who discovered the star's variabi -
lity, a companion 12.0m is present in 0.1m to W
and somewhat to the north from the variable. Can -
non points out that at Min light the variable beco -
mes fainter than the companion. No sign of the
companion's existence was found by Hoffmeister
[0016] and by Payne-Gaposchkin [0624]. Accor-
ding to [0624], the mean cycle is ~ 78d, and RVA
type is possible.
RW Ara d = 0.022P. Min II 8.91.
Changes of the shape
of the light curve due to gaseous streams or a hot
spot are possible.
TT Ara ZrO bands may be present in the spectrum
[3181].
TV Ara In the region of the cluster
NGC 6208.
TX Ara VB A (B 16.5m).
Twice shorter period is possible.
XX Ara Min II 14.1.
YY Ara The star's being
an eclipsing or irregular variable is not excluded
[0424].
AA Ara Min II 13.3.
AD Ara [A/H] = - 0.4.
AE Ara VB A (B 12m, 0.3' sf). P.K. 344 -8.1.
A compast planetary nebula
or a symbiotic star. Irregular abrupt brightenings
by 3m - 4m separated by several years are obser-
ved [0255]. The spectral data are discussed in
[8076].
AF Ara Min II 13.8.
AW Ara Before JD 2417300 Max = 2412600 + 186d*E.
BQ Ara Double maxima sepa-
rated by 10d - 20d, with Min II 12.8.
CC Ara VB;The variable is
nf component.
CH Ara Noted on the finding chart for
S 6062 = V 466 Ara.
CT Ara Before JD 2420400 Max = 2413080 + 215d:*E;
Since JD 2425000 - see Table.
DU Ara B - V: +0.52, +0.84. P var. Max = 2418145.560 +
+ 1.63999d*E (JD 2411000 - 21000); Since
JD 2425000 - See Table.
EK Ara VB A (B 15m).
EL Ara Before JD 2420400 Max = 2415140 + 332d*E;
Since JD 2425000 - See Table.
ER Ara Min II 14.2.
EV Ara Before JD 2420400 Max = 2413750 + 237d*E;
Since JD 2425000 - see Table.
EZ Ara P var.
FU Ara The depth of Min I is 0.97m and 0.89m,
the depth of Min II is 0.20m and 0.23m in blue and
yellow light, respectively.
GK Ara Before JD 2417800 Max = 2414050 + 237d*E,
Since JD 2418400 - see Table.
GM Ara Min II 12.8.
HX Ara B - V: +0.23, +0.36. A
hump on the ascending branch (fi = 0.93P) [8118].
KY Ara Only one sharp
Max (JD 2428715 - 712) was observed. Possibly
a Nova.
KZ Ara VB A (B 14.1m sp).
LP Ara d = 0.04P? Min II 10.5?
LQ Ara In
1959 rapid variations at times for 0.5m near 11m
were observed; surrounded by a nebula [4001].
LR Ara Min II 10.6.
Lu Ara Min II 10.1?
MQ Ara nf component is
variable.
MR Ara B - V: +0.72, +0.8. [A/H] = - 1.0. P var?
QR Ara Shown in the
charp for BV 1443.
QU Ara VB.
QW Ara The variab -
le is np component of the pair.
QX Ara Shown in the
charp for S 5818.
V 340 Ara B - V: +1.25, +1.68. [A/H] = 0.6.
V 341 Ara The star is blue; light va-
riations during 4d were not accompanied by
colour changes. Possibly an eclipsing varia-
ble [4678].
V 342 Ara P >= 140d.
V 344 Ara P >= 170d
V 345 Ara P >= 180d.
V 349 Ara Min II 8.8.
V 355 Ara P > 220d.
V 356 Ara P > 170d.
V 357 Ara P >= 220d.
V 360 Ara Min II 13.8:, Min II - Min I = 0.35P.
V 361 Ara Min II 13.6:.
V 362 Ara Min II 15.6:.
V 383 Ara A star 16.5m is
close to the north.
V 421 Ara Min II 15.1.
V 440 Ara Min II 14.5:.
V 444 Ara Min II 14.2.
V 454 Ara Min II 14.1.
V 480 Ara Min II 15.5:.
V 484 Ara RV
type is possible (Min = JD 2436760).
V 485 Ara Min II 14.8.
V 489 Ara Min II 11.9.
V 491 Ara Min II 11.9.
V 492 Ara Min II 14.5.
V 494 Ara RV type is not excluded.
V 501 Ara Min II 13.8.
Shown in the chart for S 6114.
V 535 Ara Min II 7.71.
Nonlinear term in the elements: -4.4d*10**-11*E**2.
V 536 Ara Min II is present.
EB type is possible. P var. P = 2.374101d
(JD 2415000 - 22000); Since JD 2422000 -
See Table.
V 539 Ara VB A (B 9.22m, 12", 269deg). Min II 6.09, d = 0.01P.
Shown in the chart for BV 1441 = V 538 Ara.
V 544 Ara 14.5m star sp.
V 609 Ara Shown in the
chart for S 5867.
V 610 Ara EA type is possible.
V 613 Ara VB (close np companion
is NSV 10198).
V 616 Ara Deep Min II.
V 620 Ara Min II is possibly present.
V 623 Ara Min II 14.5.
Twice shorter period is possible.
V 624 Ara P >= 220d.
V 625 Ara P >= 170d.
V 639 Ara VI (NGC 6397).
Probably not a cluster member.
V 651 Ara Min II 15.3.
V 653 Ara Min II 12.6.
V 656 Ara EW type is not excluded.
V 658 Ara Min II 16.0.
V 659 Ara Min II 14.4.
V 668 Ara Min II 13.8:.
V 675 Ara P >= 200d.
V 687 Ara RRC type is possible.
V 700 Ara Min II 15.7.
V 702 Ara Min II 14.0.
V 704 Ara Min II 13.3.
V 705 Ara Min II 14.4. RR type is
possible.
V 716 Ara Monotonous
brightening during JD 2436689 - 36838 was
found. The amplitude is probably greater.
V 722 Ara Min II 10.3:.
V 728 Ara Min II 12.8.
V 732 Ara CEP type is not exc-
luded.
V 743 Ara RV type is possible.
V 781 Ara Min II 14.8:.
V 783 Ara Min II 13.9:.
V 785 Ara Min II 14.3.
V 787 Ara RV type is possible.
Min JD 2436756.
V 789 Ara Min II 14.8.
V 790 Ara Min II 14.8.
V 791 Ara Min II 13.0:.
V 792 Ara Min II 15.2:.
V 801 Ara MXB 1636 - 53. Description
of the spectrum [1356].
Modulati -
on with P ~ 4h and the amplitude up to 40% was
found in the broad bAnd optical flux [4944].
V 802 Ara 14.93 - 17.03 B.
V 808 Ara EW type is possible.
V 820 Ara Epoch of Min is given. Strong mag-
netic field. Either an eclipsing binary or (mo -
re probably) an object similar to rotating vari -
ables of ACV type.
V 821 Ara 4U 1658 - 48.
Unusua1 X-ray system. Quasiperiodic optical
variations (P ~ 20s) with total amplitude 40 per -
cent, abrupt bursts on ~ 20 ms time scale lea -
ding to two-fold flux increase And light changes
by 6m during less than two months were obser-
ved [4958]. Lx/Lopt = 3.
R Ari OH emission.
T Ari P var. Max = 2417160 + 313.5d*E (JD 2404800 -
- 17200); Max = 2434616 + 323.1d*E (JD 2419400 -
- 34560). Since JD 2436560 -
See Table. = 319.53d (JD 2404800 - 44160).
Sometimes A < 1.5m.
U Ari SiO maser.
V Ari Vr = - 180 km/s.
W Ari Maps,
given in [2544, 6067] are wrong.
X Ari B - V: +0.28, +0.56. P var. Max = 2420785.635 +
+ 0.6511248d*E (JD 2420460 - 33210) [3506].
Since JD 2433210 - see Table.
[Fe/H] = - 2.17.
RR Ari Min II 6.75:; Min II - Min I = 0.55P.
Variability is not confirmed
by otHer authors' photoelectric observations. V =
= 5.75.
RS Ari Min II 11.0.
RU Ari OH emission.
RV Ari B - V: +0.29, +0.44. 0.34P =< M - m =< 0.53P. P1 = 0.07195d
[8137]; P2 = 0.27554d [7033].
Moments of brightest light
maxima T = 2435066.400 + 0.31632996d*n [2290].
RW Ari B - V: +0.35, +0.46. P var. Max = 2428183.324 +
+ 0.3543184d*E (JD 2428040 - 36700) [3188].
Since JD 2440900 - see Table.
According to
[6043] - EA type: Min I = 2439384.97 + 3.1754d*E.
Total light range (11.47 - 13.25 V) [8127]
seems doubtful. It is not excluded that the eclip -
ses and light increase of RW Ari given in [8127]
are explained by variability of one of comparison
stars used.
RX Ari d = 0.02P. Depth of Min II 0.10m.
SS Ari P var. Min II 10.82:.
ST Ari P var. Max = 2427347 + 94.2d*E (1933 - 1939); Max =
= 2429525 + 106.6d*E (1939 - 1942); Max = 2430588 +
+ 95.2d*E (1942 - 1946); Max = 2432118 + 100.0d*E
(1946 - 1961).
Mean elements are given in the Table.
SX Ari B - V: -0.10, -0.12. Epoch of Min
is given.
SZ Ari d = 0.03P.
TT Ari Porb = 0.137551d [8138].
Along
with light variations typical for Z Cam variables
there are sinusoidal variations with amplitude of
about 0.2m B and variable period: P = 0.1329d
(1961 - 62), P = 0.1327d (1966) [4931], P = 0.1326d
(1978) [4935].
Sinusoidal variations are superimposed by quasi -
periodic oscillations up to 0.2m with 8 - 20 minutes
cycle and irregular flickering up to 0.1m in 1 minute.
TU Ari P var. Max = 2420463.353 + 0.4716219d*E
(JD2420463 - 34720). Since JD2436820 -
- see Table.
TV Ari P var.
TX Ari P var?
TY Ari Form of the light curve va -
ries. Mean value of the period is given.
UV Ari The second overtone period given in the
Table is dominating. Sometimes the fundamental
period P0 = 0.062d and the first overtone period P1 =
= 0.047d are observed.
UW Ari Amplitude varies.
In the interval JD2441581 - 693 - const.
[7544].
UX Ari T = 2440133.766 + 6.43791d*E [6444],
Where T is epoch of conjunction (G5 component
is behind of Ko component).
Brightness varies in waves with a period ~
~ Porb, but the phase psi of light minimum calcula -
ted according to the elements given above changes
with time: psi = 0.1P (1972 - 1974), psi = 0.8P (1976), psi =
= 0.7P (1977), psi = 0.6P (1978).
Mean brightness varies, amplitude of the
wave varies from 0.04m up to 0.15m.
VW Ari BDS 1269 A (B 8.33m, 74", 31deg). P2 = 0.089d.
Metal deficiency. The com-
panion has normal metal abundance.
VY Ari SB? Epoch of Min is given.
Second light variation is also observed: Min =
= 2442044.6 + 43.9d*E.
A small flare in U band was
observed.
gam Ari VB A (B 4.65m, B 9 V, 7.9", 0deg).
Epoch of Min is given.
R Aur VB A (B 8.6m, 48", 239deg). P var [7165];
Cycle 64.5a is possible.
S Aur P var.
In the early forties of our century the star was faint
with small and irregular variations.
T Aur Min = 2437614.0088 + 0.20437851d*E [8145]. P var?
= 14.92, = + 0.28.
THere are light fluctuations
between the eclipses. Depths of Min are 0.10m -
- 0.28m [3195]. Faint nebula with high degree of
ionization.
U Aur H2O maser.
Y Aur B - V: +0.70, +1.06.
Z Aur P var [7110]. Max = 2425580 + 110.76d*E
(JD2416156 - 25580); Max = 2429888 + 113.35d*E
(JD2425570 - 29900); Max = 2438292 + 135.55d*E
In 1970 - irregular variations [7338]. = -165 km/s;
According to TiO bands
The spectrum is M1 [0806].
RS Aur P var.
RT Aur B - V: +0.39, +0.80. [A/H] = 0.1. P var. Max =
= 2433040.867 + 3.728365d*E (JD2417970 - 33100)
Since JD2433100 - see Table.
DV var?
RU Aur OH emission.
Mean magnitude probably varies
with Pi = 10400D [1059].
RW Aur VB A (B 12.5m, dM0e, 1", 2, 254deg).
The companion probably flares with
an amplitude 0.5m - 0.7m [3197, 3198].
Possible
period of axial rotation is 100d [7067].
OH emission.
RX Aur B - V: +0.76, +1.18; [A/H] = -0.1, P var?
Nonlinear term: -0.70d*10**-6*E**2?
RZ Aur P var. Min = 2422616.498 + 3.010593d*E
(JD2418000 - 26000); Since JD2426000 -
see Table.
SS Aur SB (P = 0.1805939D [6103]).
Sometimes abnormal behaviour of the star is
being observed when comparatively numerous and
small light maxima arise. According to [8151] the
mean cycle is 51.2d.
SU Aur Common proper motion with AB Aur (P = 3'). Associated
with a small bright nebula. OH emission.
SX Aur Min II 8.87. According to
[8153] P var: Min I = 2418218.7779 + 1.21007653d*E +
+ 0.91d*10**-10*E**2.
SY Aur B - V: +0.92, +1.23. [A/H] = - 0.3. P var [5661].
Max = 2436853.57 + 10.144330d*E (JD2417900 -
- 32380). Since JD2432380 -
See Table.
TT Aur Min II 9.0.
TV Aur S 5/6 - .
TW Aur Mean
magnitude varies with P = 1370d.
TZ Aur B - V: +0.08, +0.48. delta(S) = 2.
UU Aur VB A (B 11m, 18", 222deg).
UV Aur VB A (B 10.96m, B 9 V, 3.4", 4deg).
Bright lines [NeIII] and
[OIII] in spectrum.
UW Aur Epoch of Min is given.
UY Aur VB A (B 12m?, 0.8", 212deg). OH emission.
VW Aur VB (9.0m, 11.8m, 1.4", 332deg, 1976).
VX Aur P var?
WW Aur Min II 6.43. Min II - Min I = 0.50P.
XX Aur Min II 13.4.
YZ Aur B - V: +1.15, +1.72. [A/H] = -0.4.
ZZ Aur Min II 11.1.
AB Aur See SU Aur. Spectrum
description [4002].
AE Aur Connected with the bright nebula IC
405. The motion is directed away from Ori OB 1
association with the velocity 106 km/s.
AG Aur According to TiO bands
the spectrum is M3 [0806].
AH Aur Min II 10.70. P var.
AK Aur VB B (A = BD + 31deg 1370, 8.3m; B 82", 26deg). B - V:
+ 0.18.
AM Aur Min II 11.0. P var: Min I = 2417617.2 + 13.6182d*E
(JD2413500 - 19500) [0608]; Since
JD2425400 - see Table.
AN Aur B - V: +1.06, +1.48. [A/H] = -0.2.
AO Aur B - V: +0.86, +1.27.
AP Aur Min II 11.2. P var: Min I = 2423080.505 +
+ 0.5692965d*E (JD2423080 - 35000).
Since JD2435000 - see Table.
AQ Aur Light curve shape var?
AR Aur Min II 6.70. Min II - Min I = 0.50004P. P var: Min I =
= 2427887.7217 + 4.13467d*E (JD2427800 -
- 29500) [4999]. Since JD2438400 -
elements in the Table with an additional nonlinear
term: -2.2d*10**-8*E**2.
AZ Aur Close companion 16.3m B.
BC Aur Min II 11.7.
BF Aur Min II 9.49. P var. Min I = 2434455.3872 +
+ 1.583217d*E (JD2411760 - 34455) [5038].
Since JD2434455 - see Table.
The two sets of observations are
equally well represented by the formula: Min I =
= 2440628.3643 + 1.5832212d*E + 1.7d*10**-10*E**2
[8160].
BH Aur P var. Max = 2437352.461 + 0.45608821d*E
(JD2417260 - 42750) [7806]. Since
JD2442750 - see Table.
BK Aur B - V: +0.86, +1.26.
CI Aur Depth of Min II 0.05m. P var. Min I =
= 2439414.573 + 1.869984d*E + 0.020d*10**-8*E**2
(JD2425560 - 42045).
Elements given in the Table represent
observations in the interval JD2439052 - 40654.
CL Aur Min II 12.3; Min II - Min I = 0.45P; DII = 0.13P. P var?
Min I = 2432967.262 + 1.2443666d*E (JD2416900 -
- 32967) [0608]. Since JD2432967 -
See Table.
CO Aur The first overtone period is
given in the Table; the second overtone P = 1.4255d.
CQ Aur B - V: + 0.86, + 1.07; Min II 9.14:; Min II - Min I =
= 0.52P:; D = 0.096P. P var. Non-
linear term: +3.78d*10**-7*E**2.
CY Aur [A/H] = -0.3.
DV Aur P var. Max = 2426015 + 198.0d*E (JD2426014 -
- 27400) [0332]. Since JD2439940 -
see Table.
EI Aur Min II 15.0.
EM Aur Min II 11.7.
EO Aur Min II 7.89.
EP Aur Min II 10.9. P var?
ER Aur [A/H] = - 1.1. P var? Max = 2432951.54 + 15.69073d*E
(1949 - 1950) [1059]. In the interval
JD2443428 - 874 - see Table.
EW Aur [A/H] = - 0.6.
FF Aur [A/H] = - 0.3.
FN Aur Min II 12.3. P var?
FP Aur d = 0.080P.
FR Aur Min II 13.0.
FZ Aur d = 0.40d.
GI Aur Min II 11.7.
GK Aur Min II 14.0; Min II - Min I = 0.62P.
GO Aur P var. Max = 2426071 + 292.1d*E (JD2425505 -
- 31325); Max = 2432205 + 301.2d*E (JD2432805 -
- 36120) [3211]. Since JD2436990 -
see Table.
GY Aur Min II 13.3.
HL Aur Min II 11.0.
HN Aur In the cluster NGC 1664.
Light variations with P2 = 1400d: are
superimposed by variations with P1 = 165d:.
HP Aur Min II 11.28; Min II - Min I = 0.502P. P var. Min I =
= 2427445.400 + 1.4228180d*E (JD2427445 -
- 42683); Since JD2442712 -
see Table.
HR Aur Epoch of Min is given.
HS Aur Min II 11.2.
The value of period given in [2619] must be doubled as
the system consists of two equal components
[8164].
HU Aur Min II 12.4.
HW Aur Min II 12.6.
HZ Aur Sometimes short period
variations of Vr with the amplitude 3 km/s and of
brightness in U with the amplitude 0.02m are also
observed. Max Vr = 2439454.900 + 0.073502d*E
[5259]. P (delta(U)) = 0.07396d [4818].
II Aur Min II 15.0:.
IM Aur Min II 8.05:.
IQ Aur Epoch of Min is given.
IS Aur VB.
The range of combined brightness variation is given.
It is not known which of the components varies.
IU Aur P var. THere is an additional periodic term in the elements:
- 0.00627d*sin (2.221deg*E + 15deg). -
The ratio of Min II depth to Min I depth
is 0.78. There is secular deepening of both mini -
ma. The depth of Min I increases by 0.016m per
year. The range of light variation in the Table is
given for 1979.0 (Min II 8.69). Orbital inclination
is increasing by 0.5deg per year [5181] due to orbi -
tal precession caused by a third body. Spectrum
descriptiob [8166].
KO Aur Min II 11.2.
KR Aur = +0.10, = -0.95. SB (P = 0.1628d
[9045]). Spectrum description
[8169, 8170].
Wide hydrogen emission lines.
Long maxima and minima lasting for years are
superimposed by rapid light variations by 1 - 2m
in several days or fortnights and by 0.5m in do -
zens of seconds [8168, 8170]. The source of soft
X-rays [5191].
KS Aur VB A ( 12.5m, 5", 94deg).
KV Aur Flat waves with a cycle about 750d are so-
metimes superimposed by comparatively rapid fluc -
tuations.
KW Aur VB A (B 11.0m, 11", 1, 352deg, 1909; C 7.99m, 14.5",
226deg, 1923); SB 1 (P = 3.788568d).
Mean light level varies synchronously with orbi -
tal motion.
Besides main pulsational period there
are two more periods of nonradial pulsation:
P1 = 0.096533d, P2 = 0.088243d.
KX Aur In the IC 405 nebula.
KY Aur See KX Aur.
LY Aur VB A (B 9.1m, 0.6", 249deg, 1958). Min II 7.26; d =
= 0.017P.
MR Aur Min II 15.5.
MT Aur d = 0.02P.
NP Aur P var. Since JD2437720 - see
Table.
NU Aur Blazhko effect. Pi = 179d:.
NV Aur OH, SiO, H2O maser.
NW Aur In the region of the NGC 1893.
Min II 14.7.
According to [7160] no minimum was recorded during
visual observations covering twice all phases.
NX Aur In the cluster NGC 1893.
OP Aur In the cluster Stock 8.
OX Aur VB A (B 10.0m, 22.4", 224deg). P1 = 0.115442d.
Mean brightness
probably varies.
PY Aur Possibly a cepheid.
QR Aur Epoch of Min is given.
QY Aur SB.
V348 Aur VB A (B 13.43m, 24", 44deg).
V353 Aur During several deca-
des the star brightened by - 0.06m in a year. Pos-
sibly a planetary nebula in the process of forma-
tion.
V358 Aur In the region of the cluster
NGC 2099.
bet Aur VB A (B 14.1m, 13", 174deg). Min II 1.98.
eps Aur VB A (B 14.0m, 21", 224deg). d = 0.037P.
Survey of the physical properties of the sys-
tem [2041, 2042, 3070, 3216, 3217, 8174]. The
spectrum probably varies even outside eclipses.
The eclipses are probably due to a disk of gas
and dust surrounding the hot companion. The
brightness has physical fluctuations with the amp-
litude up to 0.24m and the cycle about 110d [2040]
which hinder revealing the possible Min II. Simi-
lar cycle was discovered also in the fluctuations
of Vr.
zet Aur Range of light variation strongly depends on lambda:
4.98 - 5.53 B, 5.36 - 7.33 U. d = 0.039P var:
37.58d <= d <= 38.07d [5486].
Light fluctuations of
K - star by 0.05m [5539].
tet Aur VB A (B 7.5m, 2", 8, 331deg, 1924).
According to
[4034] the period of magnetic field variation is
3.618D.
U Boo delta(m) var (from 0.9m to 2.4m).
V Boo P var. A strongly varies.
W Boo According to [6994], P = 30d + - .
Z Boo H2O maser.
RS Boo delta(S) = 2. P var. Before JD2435000 Max =
= 2418115.5867 + 0.37733691d*E; since
JD2435000 - see Table.
Changes of the height of ma -
xima: Max (minimal height) =
= JD2442500 + 533d*E;
a shorter cycle of changes
is possible: P ~ 58 - 62d [4832].
RU Boo B - V: +0.09, +0.44.
RX Boo H2O, SiO, OH maser.
SS Boo Depth of Min II 0.1m.
ST Boo P var. Max = 2439236.032 + 0.6222968d*E (1966 -
- 1974). Mean elements
1911 - 1974 - see Table.
Blazhko effect: Min (O - C) = 2442203 +
+ 284d*n. delta(S) = 11.
SU Boo D = 0.032P. Min II 12.04. P var.
SV Boo B - V: +0.17, +0.44. P var?
SW Boo B - V: +0.09, +0.39. P var. Before JD2426500
Max = 2421840.295 + 0.5134948d*E [2008, 2011].
Since 1960 - see Table.
Secondary oscillation: Max
(height of Max) = 2441037.33 + 12.997d*E.
According to [4833], the magnitu-
de in Max varies between 10.5 and 11.6 V.
SZ Boo P var?
TU Boo Min II 12.4.
TV Boo B - V: +0.10, +0.22. [Fe/H] = - 2.42.
Blazhko effect, Pi = 16.14d [7116].
TW Boo B - V: +0.11, +0.40. delta(S) = 12. P var. Before
JD2426890 Max = 2420340.551 + 0.53227557d*E;
since JD2426890 - see Table.
TY Boo Min II 11.35.P var.
TZ Boo Min II 10.82 (var). dII = 0.09P. P var.
Depths
of minima vary from 10.8 to 11.0 V with P ~
~ 3.5 yrs; sometimes Min II is deeper than Min I.
Some other parameters of the shape of light cur -
ve are also variable. In ~ 1960 the period chan -
ged abruptly; other period variations were also
noted.
UU Boo B - V: +0.03, +0.44. P var.
Period change ~ JD2432700 [3230].
Earlier Max = 2424967.310 + 0.45690626d*E [3229].
UW Boo Min II 10.5.
UX Boo According to [2136], delta(m) ~ 0.5m pg,
EW?
UY Boo delta(S) = 12.6. P, delta(m) var. Before JD2425500
Max = 2411459.819 + 0.6508552d*E; Max =
= 2425688.836 + 0.6507849d*E (JD2425500 -
- 28670) [1702]; Max = 2432306.759 + 0.650799d*E
(JD2428670 - 32300) [2431]. Since
JD2435900 - see Table.
VW Boo Min II 10.93. P var. Nonli-
near term: - 0.084d*10**-9*(E - 7500)**2.
WY Boo Possibly P = 90d.
XY Boo Min II 10.61. P var.
YZ Boo delta(S) = 0. delta(m) var,
The shape of the light curve varies [8186].
ZZ Boo Min II 7.44. Possib-
le radio source.
AC Boo Min II 10.55. P var?
Depth of minima and level of maxima
are variable.
AD Boo Min II 9.9.
AE Boo P var. (k - b)2 = 0.01.
AG Boo Blazhko effect is
possible.
AK Boo Min II 16.3.
AO Boo P var. Mean pe-
riod is given.
AR Boo Min II 14.5. P var.
AS Boo See AG Boo.
BD Boo See AG Boo.
BE Boo Scatter in the light curve near max light;
P var? [5264]. The value of the period in the
Table may be spurious.
BG Boo Min II 14.3.
BI Boo In the region of
the globular cluster NGC 5466.
BK Boo Min II 15.3.
BL Boo V 19 (NGC 5466). B - V: +0.12, +0.25. [Fe/H] =
= -1.35.
"Anomalous cepheid". radial velocity
cluster member.
BN Boo See BI Boo.
BO Boo The shape of the light curve vari-
es: magnitude in Max - from 14.5 to 15.0.
BP Boo 5.51 V.
BR Boo The mean light curve shows
scatter which may evidence for the necessity to
improve the period.
BU Boo See AO Boo.
The mean light curve could
not be obtained.
BW Boo Min II 7.17. Min II - Min I = 0.450P. DII = 0.06P. SB 1.
BX Boo VB A (B 10.6m, 36", 156deg). P var.
According to other sources: Min = 244076730 +
+ 0.741285d*E [7955]; Min = 2440767.26 + 0.6080722d*E
[5054].
CC Boo The star in not red.
CD Boo See CC Boo.
CK Boo Min II 9.23.
CP Boo P > 0.125d.
gam Boo VB A (B 12.5m, 33", 111deg, 1925). delta(m) var.
Radial
velocity varies with P = 0.25d +- 0.02d [4914].
kap 2 Boo ADS 9173 A (B = kappa**1 Boo, 6.69m, SB, F2V, 13",236deg).
According to [7015], P = 0.0668d (20).
Beat period ~ 16d 6086, [7015].
ksi Boo ADS 9413 AB (4.7m, G8V; 6.6m, K4V; A = 4.884",
P = 149.95A).
LiI lambda 6708 line is present in the G8V
spectrum. Both spectra show manifestations of
chromospheric activity, emissions of H and
K Ca II. Soft X-ray source. Probably it is compo -
nent A that is variable, though variability of H
and K CaII emission with the cycle 10 - 11 years
is observed for component B.
iot Boo ADS 9494 B (A 5.1m, G0; A = 3.8", E = 0.43, P =
= 225A). Min II 6.29. P var. Min = 2434132.517 +
+ 0.267812271d*E + 0.115242d*10**-9*E**2 (1916 -
1958) [3239]; Min = 2438513.4166 + 0.2678143d*E
(1947 - 1967) [8191]; since 1968 -
See Table.
Detailed
studies of period changes [5222, 7352, 7353,
8181]. Sudden period changes at JD2423800,
29300, 32300, 35150 are possible. The shape of
the light curve and the depth of Min II are also
variable. According to [2020], it is also possib-
le that ADS 9494 A is variable, with the amplitu-
de up to 0.09m.
S Cae = +0.33. P < 1d.
X Cae (k - b)2 = 0.22.
R Cam S 2/5: e. P var.
T Cam S 5/5 e.
U Cam Interfering P1 = 435.45d, P2 =
= 223.17d; P3 = 3000D [1053].
V Cam H2O, SiO maser.
Y Cam EA/SD. SB 1. Min II 10.60. P var. Min =
= 2424434.5071 + 3.3054975d*E + 0.1215d*
*sin (0.0543deg*E + 186.8deg) (JD2411400 - 33300) [0978];
Min = 2437375.4923 + 3.3055069d*E + 5.3d*10**-8*E**2
(JD2437375 - 41000) [7166]; since
JD2440000 - see Table.
The primary component is a DSCTC variable
[7166] with A <= 0.05m B. According to [4192], the
pulsational period is possibly synchronized with
the orbital motion and remains practically cons -
tant (0.066458d) during a long time interval.
Z Cam SB 2. Lower
conjunction of the G component T = 2438470.841 +
+ 0.289840d*E [5365].
Outside
outbursts the light curve is modulated with spect-
roscopic elements and has a shoulder at the pha-
se 0.88P and a broad, shallow dip at the phase
0.15P. Outside maxima flickering up to 0.5m with
P ~ 16s - 18s is observed. During maxima bright-
ness fluctuations are small [5365, 4193].
RS Cam Mean brightness varies.
RU Cam [A/H] = +0.9:. P var. Min = 2417610.1 + 22.187d*E (1908 -
- 1917), Min = 2421315.3 + 22.121d*E (1917 - 1922),
Min = 2423195.6 + 22.217d*E (1922 - 1931), Min =
= 2426350.4 + 22.138d*E (1931 - 1951), Min =
= 2433700.2 + 22.162d*E (1951 - 1961), Min =
= 2437356.9 + 22.055d*E (1961 - 1965) [3243].
Unusual variable. The shape of the light curve varies.
Before 1964 broad maxima and sharp minima were
observed; delta(m) varied by the factor of 2, with a
possible cycle 5.1a [3241]. After 1964 - 1966
delta(m) decreased abruptly (to 0.4m - 0.1m and smal-
ler), the light curve became symmetric; the me-
an light varies in the range of 0.3m B. The peri-
od varies irregularly in the interval 19.4d - 23.5d.
Groups of oscillations are observed to replace
one another, with phase shifts up to 0.5p [4206].
Unusual spectrum with intense CN and weak
C2 bands.
RW Cam [A/H] = + 0.4. P var?
RX Cam B - V: +1.05, +1.48. [A/H] = 0.
RY Cam Possibly P2 = 150.8d.
SS Cam d = 0.06P. Min II 10.35:. P var;
Nonlinear term: + 2.04d*10**-9*E**2.
SV Cam Depth of Min II 0.15m: pg. P var.
A cycle of 50a may be present in period chan-
ges. The elements in the Table are valid since
1967.5.
SW Cam P var. Before JD2437600 Max = 2434448 +
+ 254.2d*E. Since JD2440000 -
See Table.
SZ Cam Member of the
open cluster NGC 1502. ADS 2984 B (A = NSV
1458 7.1m V; B 18", 304deg). Min II 7.24, D II = 0.17P.
P var. Since 1970 - see Table;
Earlier Min I = 2427533.5191 + 2.6984166d*E
[2071].
TU Cam Min II 5.22.
TV Cam [A/H] = - 0.2.
TX Cam SiO maser.
UY Cam delta(m) var (0.2m - 0.5m V) [3528].
UZ Cam P var? Before JD2428700 Max = 2427992 +
+ 231.0d*E [0114]; Since JD2440000 -
See Table.
WW Cam d = 0.013D. Min II 11.1.
XX Cam During 1898 - 1980 a single symmetric Min
JD2429632 was observed which lasted for
94d. Brightness fluctuations up to 0.2m during
several dozens of minutes [4271]. Hydrogen
deficiency and carbon excess in the spectrum.
Some authors express doubt about the star's
being an RCB variable; in particular, they note
the lack of IR excess [5423, 5430].
AB Cam [A/H] = -0.1.
AD Cam [A/H] = -1.0.
AE Cam Min II 15.8.
AH Cam VB A (B 7"). P var. Max = 2433897.519 +
+ 0.3687404d*E (JD2427000 - 33897) [2305].
Since JD2438000 - see Table.
Magnitude in Max varies with a
possible cycle Pi = 46 P [3506].
AK Cam P var. Min = 2426393.180 + 2.226780d*E
(JD2426390 - 36610) [2594]; since
JD2436000 - see Table.
AS Cam d = 0.009P. Min II 8.97, DII = 0.06P, Min II - Min I =
= 0.437P.
AT Cam Min II 10.6.
AU Cam Very red.
AV Cam d = 0.04P.
AW Cam Min II 8.36.
AX Cam Detai-
led spectral studies [7191], [7192].
AY Cam Min II 10.23, DII = 0.12P, dII = 0.02P.
According to [3260], the
spectrum is A5.
AZ Cam Min II 10.8.
BI Cam delta(m) = 0.9m pg.
BK Cam During 1912 - 1932 periodic
(P ~ 4.4a) spectral changes were observed
which came to an end by 1937 [4282].
BM Cam SB 1 (P = 80.174469d; e = 0.35).
Epoch of Min light is given.
R Cnc SiO maser.
S Cnc In the field of Prae -
sere (NGC 2632) cluster. d = 0.015P. Min II 8.39.
P var.
U Cnc VB A (B 3"). In the
field of Praesepe (NGC 2632) cluster.
V Cnc S 0.5/6e. ADS 6763 A (B 13.5m, 10", 270deg).
RS Cnc P2 = 1700d. Tc lines are
present in the spectrum.
RT Cnc P2 ~ 600d.
RU Cnc d = 0.035P. Min II 10.21:, DII <= 0.07P.
RW Cnc P var. Since JD2437000 - see
Table.
According to [2088], Max = 2421339.380 +
+ 0.5471932d*E + 0.57d*10**-9*(E - 5800)**2 + 0.028d*
cos 0.0215deg*(E + 2260) + f(psi, hi); here the last term
is the sum of two short period oscillations and
is given in graphical form, since the main period
(0.547d) varies with Pi1 = 29.9d and Pi2 = 91.1d.
Magnitude in Max varies from 10.7m to 11.8m, in
Min from 12.3m to 12.6m.
RY Cnc In the region of the
open cluster NGC 2632 (praesepe), non-member.
B - V: +0.58, +1.05. P var. Before JD2436000
Min = 2429334.445 + 1.0929500d*E; since
JD2436000 - see Table.
RZ Cnc Min II 9.21. d = 0.015P:.
Ellipsoidal components.
SS Cnc delta(S) = 1.2. P var?
SV Cnc B - V: + 0.10, + 0.52.
SY Cnc Flickering with P ~ 20s - 34s [5959].
Spectral investigation [4286].
TT Cnc (k - b)2 = 0.11. P var. Before JD2430700
Max = JD2425647.452 + 0.5634445d*E [3506].
Since JD2439800 - see Table.
Blazhko effect, Pi = 89d [5271].
TW Cnc d = 0.014P. Depth of Min II 0.1m pg.
TX Cnc Member of the
open cluster Praesepe (NGC 2632). Min II 10.32.
TY Cnc d = 0.013P. P var.
UU Cnc Min II 9.2, JD (Min II) 2435608.5. SB 1.
The light curve is uns-
table. Spectral studies [1881], [3149], [4289].
UV Cnc In the region of the
Praesepe (NGC 2632) cluster.
UZ Cnc Min II 11.4.
VY Cnc Min II 12.3:.
VZ Cnc (k - b)2 = 0.32.
Beat phenomenon for two oscillations is
observed. According to [2125], for the middle of
the ascending branch T (m~) = 2433631.84615 +
+ 0.17836376d*E + 0.00193d sin 2 pi psi (m~) -
- 0.00371d cos 2 pi psi (m~); Here the phase of the beat
period psi (m~) is computed with the elements T (m~) =
= JD2433631.8421 + 0.716292d*E. See also [2124].
Spectral investigation [2126].
WW Cnc According to [7531], the period do-
es not vary since 1933. A number of minima by
BBSAG contradict the tabulated elements.
WX Cnc Min II 10.7.
WY Cnc VB A (B 12.8m, - 20", 0deg). Min II 9.60.
XX Cnc See UV Cnc.
XZ Cnc Min II 10.2.
YY Cnc According to [3263], the star is probably an irregu -
lar variable.
YZ Cnc Oscillations with P = 133.2m are obser -
ved in maximum light [6249].
ZZ Cnc d = 0.02P:.
AC Cnc Min II 14.7. = 14.5.
The brightness outsibe eclipses varies in the range 13.8 -
- 15.2B. 3 deep minima contradict the tabulated
elements [4460]. The identification with the X-ray
source H 0857 + 13 is not excluded.
AD Cnc Min II 13.4.
AH Cnc Member of the open
cluster M 67 (NGC 2682). Min II 13.68.
Nonlinear term: + 1.56d*10**-10*E**2.
Cyclic period variations
(with different cycles) are also possible [4475].
AO Cnc Min II 13.4.
AP Cnc P var?
AU Cnc Possible mem-
ber of the cluster praesepe (NGC 2632).
AV Cnc - AZ Cnc
See AU Cnc.
BB Cnc delta(mu) > 6.0. See AU Cnc.
BC Cnc delta(mu) > 4.0. See AU Cnc.
BD Cnc - BE Cnc
See AU Cnc.
BG Cnc - BH Cnc
See AU Cnc.
BI Cnc The elements were determined by
Winzer. Epoch of Max in U band is given.
BK Cnc See AU Cnc.
BM Cnc SB (P = 585.4154d [6568]).
The elements in the Table represent the moments of
maximal (B - V).
BN Cnc Member of the cluster Pra -
esepe (NGC 2632).
BQ Cnc SB see BN Cnc.
BR Cnc VB A (B 14.2m, 30", 268deg). See BN Cnc.
BS Cnc See BN Cnc.
BT Cnc See BN Cnc.
Oscillations with other pe -
riods are superimposed.
BU Cnc See BN Cnc.
According to [4483], P = 0.071d is not confirmed;
during different nights P = 0.0534d, P = 0.059d and
several other periodicities were observed.
BV Cnc - BY Cnc
See BN Cnc.
BZ Cnc See UV Cnc.
CC Cnc Cycle <= 90d.
CD Cnc See AU Cnc.
CE Cnc - CH Cnc
See UV Cnc.
CI Cnc See AU Cnc.
CK Cnc - CL Cnc
See UV Cnc.
CM Cnc - CN Cnc
See AU Cnc.
CO Cnc - CP Cnc
See UV Cnc.
CR Cnc - CS Cnc
See UV Cnc.
CU Cnc G 9 - 8 = G 40 - 25. VB A (B = CV Cnc, 13", 347deg),
common mu.
In the region of Praesepe
(NGC 2632) cluster, non-member.
CV Cnc G 40 - 26. See CU Cnc.
CY Cnc See BN Cnc.
CZ Cnc Equinox in [8354] must be 2000.0.
DD Cnc See UV Cnc.
DF Cnc See UV Cnc.
Possibly non-member.
DG Cnc See DF Cnc.
DH Cnc - DI Cnc
See AU Cnc.
DL Cnc VB. See UV Cnc.
DM Cnc See AU Cnc.
DN Cnc - DP Cnc
See UV Cnc.
DQ Cnc See DF Cnc.
DR Cnc See UV Cnc.
DS Cnc See DF Cnc.
DT Cnc - DU Cnc
See UV Cnc.
kap Cnc SB (P = 6.39316d).
In [4487] the light variabi-
lity was not confirmed.
R CVn P var. Max = 2411768 + 325.4d*E (JD2411730 -
- 26430) [1701]; Max = 2432074 + 332.8d*E
(JD2426750 - 32100); since JD2432100
- see Table.
T CVn SRA? delta(m) strongly varies.
U CVn OH, H2O emission.
V CVn H2O, SiO maser.
W CVn B - V: +0.15, +0.42. P var.
Nonlinear term: -368*10**-13*E**2. delta(S) = 7.
Y CVn P2 = 2000d.
Z CVn B - V: +0.20, +0.33. P var. Max = 2413000.262 +
+ 0.6538236d*E (JD2413000 - 23170); Max =
= 2423860.355 + 0.6539052d*E (JD2423860 -
- 31800) [1702]; Max = 2432943.645 + 0.653824d*E
(JD2431800 - 40200) [6457]. Since
JD2438900 - see Table.
Blazhko effect: Min. ampl. = 2439176.12 +
+ 22.75d*E [3267].
Amplitude varies by 0.5m B, extremal periodic de-
viations of the epoch of Max from linear ele-
ments are + - 0.02d. delta(S) = 8.
RR CVn B - V: +0.09, +0.45. [Fe/H] = -1.33.
The light cur -
ve shape and delta(m) var.
RS CVn Min II 8.19; Min II - Min I = 0.506P; d = 0.033P.
P var. Nonlinear term:
- 1.00d*10**-8*E**2.
Wave-like distorsion with the amplitude from
0.09m up to 0.20m and with the period 4.7917d clo -
se to the orbital one is observed on the light
curve out of eclipses [7209]. The wave is migra -
ting on phase in the direction of phase decreasing
with a migration period of 9.48 years [5800].
RU CVn B - V: +0.10, +0.39. P var. Max = 2420227.338 +
+ 0.5732502d*E (JD2418801 - 29436) [5436]; Max =
= 2420227.398 + 0.57324647d*E (JD2418979 -
- 36665) [3271]; since JD2434483 -
see Table.
RV CVn V 141 (M3/NGC 5272). Not
a member of the cluster. Min II 15.81.
RX CVn B - V: +0.17, +0.41. P var?
RZ CVn B - V: +0.12, +0.43. P var. Max = 2424621.489 +
+ 0.56740036d*E (JD2424620 - 31000) [0188];
Max = 2437823.433 + 0.5674174d*E (JD2434470 -
- 37830); since JD2438200 -
see Table.
ST CVn P var? delta(S) = 4.8.
SV CVn P var. Max = 2427434.911 + 0.66805653d*E
(JD2426000 - 32000) [0752]; since
JD2439500 - see Table.
SW CVn P var. Max = 2431139.791 + 0.44164922d*E
(JD2425640 - 32000) [0752]; since
JD2436200 - see Table.
TX CVn SB 2 (P = 70.8d) [4504].
UU CVn In the region of
the globular cluster NGC 5466. P var. Max =
= 2437817.312 + 0.5409589d*E (JD2436360 - 39945);
since JD2439945 - see Table.
UV CVn In the region of globular cluster
NGC 5466, non-member. P var. Max = 2419446.156 +
+ 0.6316090d*E (JD2419440 - 34455); since
JD2434450 - see Table.
UW CVn In the region of
the globular cluster NGC 5466.
UX CVn Min II 11.94. U - B: -1.05, -0.99; B - V: -0.29,
-0.23.
VV CVn Min II 14.3:.
VW CVn Min II 12.4. P var. Min I = 2435923.246 + 0.8499757d*E
(JD2427900 - 36000); since JD2435900 -
- see Table.
The variable is not mar -
ked on the map. It is by 6mm to the west and
3mm to the north of the comparison star C.
VZ CVn Min II 9.54.
WW CVn Blazhko effect is possible.
WY CVn V 205 (M3/NGC 5272). Member
of the cluster? See WW CVn.
WZ CVn V 206 (M3/NGC 5272).
Non-member? Blazhko effect.
XX CVn In the region of M3 (NGC 5272)
Globular cluster. Member of the cluster?
YZ CVn d = 0.055P, Depth of Min II 0.05m
vis.
AA CVn [Fe/H] = - 1.78.
AD CVn [Fe/H] = - 1.39.
AF CVn [Fe/H] = - 1.19.
AG CVn [Fe/H] = - 2.01.
AH CVn [Fe/H] = - 2.01.
AI CVn Radial multiperiod pulsations: P0 = 0.2085d,
P1 = 0.1529d, P2 = 0.1259d, P3 = 0.1158d.
AK CVn [Fe/H] = - 1.19.
AM CVn The light curve is a
double wave. Min II sometimes disappears. The
depth of Min I changes also. Epoch of Min I is
given in the Table. P var; dP/dT = + 0.012s per
year. Elements for 1978 are given in the Table.
The brightness fluctuates with the cycle of
115 - 120s, sometimes the periodicity with P =
= 26.3s is observed. Probably it is a close bina -
ry semidetached system of two white dwarfs
with an accretion disk and a hot spot.
AN CVn [Fe/H] = - 1.54.
AQ CVn Similar to horizontal branch
stars in globular clusters. A flare lasting 20
minutes was observed.
BF CVn G 123 - 75 = G 164 - 32. VB A (B = G 164 - 31, 13.16m,
dM3.5e; 17", 225deg).
Flares
in the combined light of the system (delta(U) up to
0.95m) were observed.
BG CVn P1 = 1186s, P2 = 780s.
BH CVn SB. Reflection effect delta(m) =
= 0.013V.
BI CVn Min II 10.70. P var?
alf 2 CVn
VB A (B 5.60m, F0V, 19.6", 228deg).
Epoch of Min is given.
R CMa Min II 5.78. P var [3280, 6314].
The star shows
anomalies of the light curve [3281, 3282].
V CMa VB B (A = CPD -31deg 1311, 9.4 m; B 16", 90deg).
Z CMa Strong IR excess. Shell spectrum. Several lines
show P Cyg profiles. The star is located in a
nebula rich in details. A bright wisp of nebu -
losity near the star has continuons spectrum,
probably identical to that of the star [4002].
RR CMa Min II 13.1.
RT CMa Min II 11.5.
P = 1.293745d is possible ta-
king into account the epoch from [3283].
RX CMa d = 0.027P. Min II 11.1. P var. During
JD2441700 - 43000 - see Table.
RZ CMa P var? since JD2435500 -
see Table.
SW CMa Min II 9.9. Min II = JD2426709.366; Min II - Min I =
= 0.316P.
SX CMa Min II 10.3.
TU CMa Min II 10.1.
UW CMa Min II 5.25.
Gaseous streams,
expanding gaseous envelope. Minima are asym-
metric; other peculiarities of the light are obser-
ved. A number of spectral lines have P Cyg profiles.
The line profiles are observed to vary with
the phase of the orbital period, and also ([7227],
according to Sanyal) with characteristic time
<1h.
UX CMa Min II 12.3.
VW CMa Min II 9.1.
VY CMa ADS 6033 A (B 9.2m, 0.5", 168deg; C 11.5m, 2.7", 291deg,
D 11m, 2.9", 347deg, ...). H2O, OH, SiO maser.
B - V: +2.3.
In the region of the
young open cluster NGC 2362. Embedded in a
reflecting nebula. The companions may be details
of the nebula;some of them are probably va-
riable [2159, 3287]. Surrounded by an envelope
of gas and dust or a disk of 0.45" (lambda = 5 mkm) angu-
lar size. Secular decrease of brightness since
1801. Cyclic variations of brightness with delta(m)
from several tenths of a magnitude to 3m on ti-
me scale from 200d to 1900d. TiO And ScO emis-
sion bAnds in the spectrum. Spectroscopic stu-
dies [3287, 5282, 6133].
WW CMa RR, Max = 2428570.09 + 0.499355d*E [0613]. CEP,
Max = 2428146.6 + 5.7660d*E [0514].
These systems of
elements are contradicted by 94 photographic
observations (Erleksova) and 12 photoelectric
observations (Irwin, [3288]).
XY CMa d = 0.04P:.
ZZ CMa Min II 13.0.
AE CMa d = 0.02P:.
AN CMa d = 0.02P:.
AO CMa In the field
of the open cluster Ruprecht 18.
AR CMa d = 0.025P:.
AS CMa d = 0.04P.
BN CMa Min II 14.9.
BQ CMa In the region
of the open cluster NGC 2354.
BS CMa Min II 14.5.
CC CMa Mean brightness varies?
CE CMa Min II 13.3. Min II - Min I = 0.663P.
CH CMa Min II 12.9.
CK CMa Min II 15.4.
CM CMa Min II 13.1.
CO CMa Mean brightness probably varies with
P ~ 700d.
CR CMa Min II 12.4.
CV CMa Min II 13.5. DII = 0.09P. Min II - Min I = 0.358P.
CW CMa Min II 8.94. SB 2.
CX CMa Min II 10.3.
DD CMa Min II 11.8.
DE CMa Min II 13.4.
DS CMa VB A (B 15.8m, 10", 130deg).
DV CMa JD2425300 - 27500: P - see Table;
since JD2428000 P ~ 400d.
EF CMa d = 0.02P.
EW CMa VB (delta(m)) <= 0.5m, 0.102", 112.1deg, 1952.203).
SB (P = 0.261975d).
Brightness variations are not related to the or-
bital phase. Shell star (probably an extended at-
mospHere of one of the components and the com-
mon shell around the system). Spectral studies
[4592 - 4596].
EX CMa Was faint for 2 nights (October 8 and 9,
1962).
EY CMa P var, delta(m) var [3960].
The main wave is super-
imposed by secondary ones (P = 0.2033d and
0.1690d); beat effect, Pb ~ 2.00d [7243].
EZ CMa SB. In the centre of
the ring HII region S 308. Member of the open
cluster collinder 121. Epoch of Max light is gi-
ven. The companion is probably a neutron star.
The shape of the light curve, delta(m), phases of ma -
xima and minima and mean light vary from one
observational season to anotHer.
FF CMa Min II 7.6. Elements
should be improved. Member of the open cluster
Cr 132a.
FM CMa Min II is almost as deep as Min I [6585].
FN CMa VB (6.3m, 7.5m, 0.561", 115.8deg, 1978.15).
Range of combined light variation is given in the Table.
Asociated with the nebula vB 95. According to
[6135], The period considerably differs from the
tabulated value.
FQ CMa Min II 9.7.
FR CMa ADS 4978 AB (6.2m, 10.4m, 4"23deg; C 11.62m, 56").
FS CMa Extended shell of gas and dust. Emissions of
[FeII], [NiII], [CrII], [SII], [OI], FeII.
IR excess (1.6 - 20 mkm). P Cyg profiles of
Balmer lines vary in the time scale of hours.
Brightness varies from night to night by 0.1m and
during a night by 0.03m, sometimes in correlati-
on with spectral changes [6636]. Spectral studi-
es [7250, 7251, 7253].
FT CMa VB A (B 12.58m, 36", 97deg).
FU CMa VB A (B 14.7m, 14", 230deg, 1897; C 11.07m, 40", 225deg).
FW CMa VR var, P = 31.9045d [6154].
FZ CMa Min II 8.44. In the HII region
S 295, in the association CMa OB 1.
GG CMa Member of the open
cluster Cr 132a.
GU CMa ADS 5713 AB (7.5m, 8.2m, 0.6", 187deg, 1919). SB?
In the HII region S 293.
GY CMa According to [8380], does
not vary.
GZ CMa SB 2.
HK CMa Epoch of Min is given.
HL CMa 1E 0643.0 - 1648. SB (P ~ 0.217d); Lx/Lopt var
(0.002 - 1).
bet CMa In 1971 - 72 the observations were
described by the combination of the tabulated
elements (period P1) and the following systems
of elements: Max = 2441296.0705 + 0.251300d*E, (P2);
Max = 2441296.032 + 0.23904d*E, (P3); Max =
= 2441296.065 + 0.12501d*E, (P1/2); Max =
= 2441296.124 + 0.12565d*E, (P2/2).
Beat periods: 49.198d, 5.442d, 4.900d.
Since 1908
P1 increases, P2 decreases.
12 overtone and resonance periods were
found in [3454].
ksi 1 CMa
ADS 5176 A (B 14.5m, 25", 147deg; C 14.0m, 29", 303deg,
1897).
sig CMa ADS 5719 A (14.2m, 11", 153deg, 1926).
ome CMa SB?
R CMi SC 4/10 e.
T CMi P var. Max = 2422456 + 324.2d*E (JD2416610 -
- 22800); Max = 2430896 + 311.2d*E (JD2423090 -
- 30900); Since JD2430900 -
see Table.
U CMi There is a hump on the ascending branch looking
sometimes as a secondary maximum. The light
curve for 1904 - 1970 [7368].
X CMi P var? delta(S) = 3.
RS CMi d = 0.02P:.
RX CMi Min II 14.6; Min II - Min I = 0.52P:.
RY CMi Min II 12.0:.
SX CMi DI <= 0.12P. Min II 13.6.
SY CMi P var. Max = 2425234.682 + 0.565900d*E (JD
2425234 - 708); since JD2436586-
see Table.
TU CMi Min II 15.1.
TW CMi Min II 15.6.
TX CMi Min II 14.7.
UZ CMi Min II 12.1.
XZ CMi Min II 9.88. P var?
YY CMi Min II 8.88.
YZ CMi mu = 0.604", P = 221.4deg.
Epoch of Min is given. P var; additional
term: - 0.00003919514d*E (E + 1)/2. Periodical
light variations with the amplitude 0.12m (11.26 -
- 11.38 V) are superimposed by strong flares.
AG CMi P var. Min = 2434698.670 + 1.6645729d*E (JD2426350 -
34740) [1727]. Since JD2437650 -
see Table.
AH CMi EW?
AK CMi Min II 10.3; Min II - Min I = 0.55P. P var. Min I =
= 2425352.348 + 0.56589534d*E (JD2424880 -
- 35550) [1728]. Since JD2435600 -
see Table.
AL CMi Observations in
the interval JD2424880 - 25950 are represented
by the elements: Max = 2425243.631 + 0.55050d*E.
Since JD2436590 - see Table.
AM CMi Min II 10.5.
AN CMi d = 0.02P:.
AO CMi d = 0.01P:. Min II 14.5.
BF CMi Depth of Min II 0.05m:.
RS Cap Mean
brightness varies with P = 3360d.
RT Cap VB A (B 15m, 26", 227deg).
RU Cap VB A (B 13.6m, 1.6", 86deg).
RV Cap var: Max = 2424334.6612 + 0.44775262d*E
(JD2417400 - 33610) [0323]. Since
JD2433850 - see Table.
Light curve and period vary with the
Blazhko effect period Pi = 225.5d [6464]. Semi-
amplitude of deviations from linear elements is
+- 0.032d. 0.14P <= M - m <= 0.25P. (k - b)2 = 0.05.
RW Cap d = 0.020P. Min II 9.9. P var. Min I = 2418924.594 +
+ 3.3923922d*E (JD2418920 - 24000) [6774];
Min I = 2424003.014 + 3.3923457d*E (JD2424000 -
- 34500) [2389]; since JD2435400 -
see Table.
RX Cap Min II 12.5.
RY Cap VB B (A 7.1m, F0; B 6.6", 90deg; C 12.0m, 8.5", 58deg).
TV Cap
= 67d [1331].
TW Cap P var. P = 28.6421871d (JD2414000 - 17600);
P = 28.61700115d (JD2417600 - 24000) [1331];
Max = 2426211.90 + 28.59497d*E (JD2421400 -
26200) [2390]; Max = 2435664.8 + 28.5578d*E
(JD2426210 - 37500) [2309]; since JD
2437500 - see Table. 0.14P <= M - m <= 0.40P.
[Fe/H] = - 0.72.
TY Cap Min II 10.6. P var.Min I hel = 2432017.956 +
+ 1.423466D*E (JD2425500 - 35000);
since JD2435000 - see Table.
UW Cap Min II 11.5; Min II - Min I = 0.5P. P var? Min I =
= 2434627.290 + 1.399118d*E (JD2427000 - 35000);
since JD243500 - see Table.
YZ Cap (k - b)2 = 0.08.
AD Cap Outside eclipses
B - V = +1.00. P var?
AE Cap Mean
brightness varies with P = 2300d.
del Cap VB A (B 15.8m, 69", 94deg; C 12.7m, 119", 302deg,
1911); mu = 0.391", P = 138.8deg. Min II 2.90.
The light curve shape var? [3305].
eps Cap VB A (B 9.52m, 68.7", 47deg).
R Car VB A (B 12m, 2.1", 138deg). H2O, SiO maser.
U Car P var. Max = 2429023.80 + 38.753d*E (JD2415000 -
29500); since JD2429500 -
see Table.
V Car The light curve shape var?
X Car Min II 8.6.
Y Car VB A (B 12.22m, 15"; C 12.96m, 30"). SB (P = 400 -
- 600D) [5119].
The funda-
mental mode period P0 is given in the Table.
(A = 0.58m). The first overtone period P1 = 2.55954d
[5119] (A = 0.28m). P1:P0 = 0.7032.
RR Car P var.
= 154d (JD2421500 - 23500);
= 259d
(JD2426400 - 30100);
= 154D (JD2430400 -
- 33100). S 6.5/1**- .
RT Car In the region of the cluster
Tr 15.
RY Car There is a close com-
panion 14.3 pg. P var. Max = 2418475 + 416d*E
(JD2415140 - 18500); Max = 2429901 + 417.3d*E
(JD2423600 - 32900); since JD2434100 -
see Table.
ST Car Depth of Min II 0.27m.
SW Car Depth of Min II 0.05m.
SZ Car In the region of the cluster
NGC 3114.
TX Car The light curve shape var?
TZ Car Mean brightness varies with P = 1183d; the amp-
litude of the short cycle is large in mean bright-
ness maximum and small during its minimum.
UX Car In the region of the cluster
IC 2581.
VV Car In the region of the very poor cluster
N 99 [7374] (10h 36.0m -58deg 56', 1950.0) embedded
in a nebula.
VY Car VB A (B 11.07m; B 9V:, 10", 150deg). P var.
Nonlinear term: - 0.000021d*E**2
(JD2410000 - 44200).
The latest observations may be represen-
ted also by linear elements: Max = 2444161.16 +
+ 18.9138d*E (JD2441000 - 44200). [A/H] = 0.4.
WZ Car P var. Max = 2419981.099 + 23.000945d*E (JD
2410000 - 20000) [0025]; Max = 2423984.12 +
+ 23.0054d*E (JD2419800 - 25500) [0322]; Max =
= 2434914.86 + 23.0075d*E + 0.000025d*E**2 (JD
2434500 - 41200) [2309]; since JD2434500 -
- see also Table.
XX Car P var. Max = 2420769.703 + 15.723704d*E (JD
2410000 - 22500) [0025]; P = 15.7196d (JD
2423000 - 30000) [0003]; since JD
2434500 - see Table;
Elements given in the Table contain a nonline-
ar term: -0.0000034d*E**2.
XY Car [A/H] = 0.1.
XZ Car [A/H] = 0.2.
YZ Car P var. Nonlinear term:
+ 0.0000022d*E**2. [A/H] = - 0.1.
AE Car In the region of the cluster
NGC 3532.
AF Car P var. Max = 2434532 + 433.7d*E (JD2420200 -
- 34600); since JD2435000 -
- see Table.
AG Car Central star of the low-excitation plane-
tary nebula P.K.289 - 0.1 ejected probably during
a nova-like outburst of the star adout 1000 years
ago [7052, 7113].
AS Car d = 0.025p.
AW Car d = 0.015p.
BL Car In the region of the cluster
Tr 16.
BO Car VB A (B 11.05m V, B8III, 10", 41deg). See
RT Car. Cluster non-member.
BP Car P = 4.82246d?
BS Car In the region of the clus -
ter IC 2602. Min II 15.3.
BZ Car Mean brightness possibly varies with P = 1800d.
CD Car In the centre of the cluster
Cr 236.
CF Car The region of the cluster
NGC 3496.
CI Car In the region of the cluster
NGC 3572. d = 0.021P?
CO Car d = 0.024P?
CV Car d = 0.046P. Depth of Min II 0.05m.
DE Car d = 0.016P?
DH Car VB B (A 15.2m V; B 13", 350deg). B - V = +0.90m
(Min brightness).
DI Car Besides cep-
heid-like light variations with the amplitude
1.7m and elements Max = 2438553.70 + 29.210d*E
(JD2438465 - 40300) [5324] large weakenings of
brightness are observed [4678]. At Max B - V =
= + 1.34.
DK Car d = 0.07P.
DM Car d = 0.040P.
DP Car d = 0.034P. Min II 13.1.
DS Car d = 0.03P.
DU Car In the region of the cluster
IC 2602.
DW Car In the region of the cluster
Cr 228. Min II 10.3.
EF Car d = 0.04P.
EG Car See AE Car.
EH Car VB A (B 15", 320deg).
EK Car See AE Car.
EM Car Min II 8.9.
EN Car In the region of the clus-
ter Tr 18.
EQ Car d = 0.030P. Min II 13.7.
ER Car See AE Car.
ES Car In the region of the cluster
NGC 3572.
EZ Car Min II 9.8.
FI Car P var. Max = 2425446.81 + 13.4542d*E (JD
2423790 - 35300) [0046, 2309]. Since
JD2435300 - see Table.
FK Car VB.
FO Car VB A (B 14m, 7", 90deg). P var. Max = 2434922.531 +
+ 10.3559d*E (JD2423700 - 35300) [6006];
since JD2436000 - see Table.
B - V: +1.13, +1.43.
FP Car d = 0.01P:.
FQ Car See EN Car.
FS Car See VV Car. Min II 10.9.
FT Car According
to [2197] spectrum C. Misidentification is pos-
sible.
FV Car VB A (B 13m, 10", 135deg). P var.
There are two additional terms in the
elements given in the Table: - 0.1065d*10**-7*E**2 -
- 0.584d*10**-11*E**3. d = 0.02P:. Min II 13.0.
GG Car Min II 9.5. Gas
and dust envelope.
GH Car See EN Car.
GK Car In the region of the clus-
ter Tr 19. Min II 13.2.
GL Car See ES Car. Min II 10.31.
System with the apsidal mo-
tion; E = 0.157, omega = 99deg.
THere are sinusoidal terms in
the elements for Min I given in the Table:
+ 0.121d sin (0.094389deg*E) - 0.007d sin (0.188778deg*E);
Min II = 2424263.236 + 2.4222338d*E -
- 0.121D sin (0.094389deg*E) - 0.007d sin (0.188778deg*E).
DII = 0.17P.
GM Car See VV Car. Min II 9.22.
GN Car Min II 12.1.
GO Car VB A (B 15", 60deg).
GP Car Min II 12.8.
GQ Car Min II 13.5.
GR Car Min II 14.0; Min II - Min I = 0.316P; DII = 0.05P.
GV Car Possible member of
the cluster NGC 3532. Min II 9.1.
GW Car Min II 9.9.
GZ Car Light elements for the fundamental mode oscilla-
tion with an amplitude 0.16m are given in the
Table.
For the first overtone oscillation with an ampli-
tude 0.07m Max = 2440742.4 + 2.93424d*E.
Epochs of maxima and amplitudes are gi-
ven according to [5175].
HH Car VB A (B 13.0m, 5", 260deg; C 11.11m, 13", 337deg;
D 12.65m, 15", 7deg). d = 0.02P. Min II 10.66. P var
[8094]. Min I hel = 2430860.162 + 3.2315393d*E
(JD2427590 - 35260) [5292].
Possible current
elements are given in the Table.
HI Car Min II 10.8.
HK Car VB A (B 12.5m, 4").
Range of combined
brightness variation is given.
HL Car d = 0.03P:.
HN Car Min II 12.5.
HP Car VB A (B 9.1m, 0.4", 178deg). Min II 9.3.
Elements should be
corrected [8083].
HQ Car B - V: +0.63, +1.04.
HR Car Spectrum description 1914,
[6466].
HT Car In the region of the cluster
IC 2581. Min II 14.0.
HV Car d = 0.026P. Min II 14.2.
HW Car Epoch of Min is given.
HX Car Min II 14.5.
IK Car See DU Car.
IL Car Min II 14.4.
IN Car It is possib-
le that the period must be doubled.
IQ Car See AE Car.
IR Car See AE Car. Min II 12.6.
IS Car Min II 14.0.
IU Car (k - b)2 = 0.02.
IW Car Mean brightness varies with the period close to
1500d, the amplitude of main oscillations - from
1.3m to 0.3m.
IX Car In
the centre of a bright nebula with the diameter 2.4'.
KQ Car Min II 10.3.
KU Car Min II 11.6.
MP Car VB A (B 16m, 180deg).
MZ Car Sf component of
a close pair.
OO Car Min II 14.7.
OV Car Min II 13.5.
OY Car Eclipse elements:
Min I hel = 2443993.553241 + 0.0631209247d*E
[5185]; D = 0.050P, d = 0.044P.
The hump on the light
curve is observed at the phase of 0.75P.
Depth of Min I varies between 1.48m and 2.47m.
PT Car Min II 13.0:.
PX Car Min II 10.10.
QR Car Min II 10.4.
QS Car Min II 9.3.
QU Car HDE 310376 (HA 112, 173).
Flicke-
ring resembles V818 Sco. Variations by 0.2m in 90s
were observed. No periodicity was found. Emis -
sion lines He II 4686, CIV - NIII 4630 - 4650 and
sometimes weak hydrogen absoptions (correspon-
ding to A or B type) are noticeable in the spe-
ctrum [5643].
QX Car Min II 7.02.
QY Car In the open cluster
No.90 [7374].
QZ Car In the eta Carina nebula,
possible member of the cluster Collinder 228.
Min II 6.43.
Two SB 1 systems (A and B),
B is eclipsing (A: SB 1, P = 20.73d, O9.5 I,
delta(m) = 0.6m). Combined brightness is given.
V 341 Car In the variable
reflecting nebula IC 2220. In the region of the
open cluster NGC 2516. IR excess.
V 343 Car VB. SB (P = 133.92d).
V 347 Car Deep Min II.
V 348 Car In the open cluster
IC 2581. Min II 8.9.
V 354 Car Very red.
V 356 Car Member of the cluster
NGC 2516.
V 357 Car SB (P = 6.74483d [4627]).
V 361 Car In the region of the clus-
ter NGC 3293.
V 365 Car See AE Car.
V 367 Car Min II 7.54.
V 373 Car See V 356 Car.
V 374 Car See V 356 Car.
V 375 Car P = 0.264d or 0.359d.
V 376 Car VB A (B 6.83m, B 9.5V, 41", 75deg).
V 378 - V 381 Car
In the open
cluster NGC 3293.
V 382 Car In the region of the clus-
ter NGC 3532.
V 385 Car Depth of Min II 0.04m.
Surrounded by a ring
nebula RCW 58.
eta Car In the
emission nebula NGC 3372 in the region of the
cluster Tr 16. A very massive young star surro-
unded by an expanding gas and dust shell with
the diameter 2" at 2mu and 6.5" at 12.2mu. Maxi-
mum brightness was observed in 1843. Since
1880 varies in the range 5.9 - 7.9 V. In the inter-
val JD2434000 - 41000 Max = 2434037 + 1110d*E.
there are emission lines of H, HeI, FeII, [FeII],
etc. in the spectrum. Description of the spectrum
[5251, 7279]. Soft X-ray source of variable inten-
sity.
HI Car Soft X-ray source.
R Cas VB A (B 14.5m, 14", 273deg). SiO, OH maser;
Sometimes H2O emission.
T Cas SiO maser.
ZrO bands in the infra-
red spectral region.
U Cas S 4.5/4e.
W Cas SC 5/9e.
X Cas P var: Max = 2426650 + 432.32d*E (JD2416750-
- 27060); Max = 2432870 + 413.6d*E (JD2427060-
- 32870); Max = 2437948 + 423.0d*E (JD2432870-
- 39210).
Current elements are given in the Table.
Y Cas OH, H2O emission; SiO maser.
Z Cas SiO maser.
RS Cas P var. Max = 2416942.16 + 6.29552d*E (JD2412650-
34900) [3317]. Since JD2434900 -
see Table.
RV Cas There
are signs of Se type in the spectrum [3383].
RW Cas P var. Max = 2421354.22 + 14.8004d*E (JD2417000 -
- 30000). Since JD2430000 -
see Table. [A/H] = 0.3.
RX Cas Unigue rapidly evolving eclipsing
system. Min II 9.49; Min II - Min I = 0.5070P. P var.
Nonlinear term:
+ 1.017d*10**-5*E**2.
Observati-
ons may be represented also by three systems of
elements: Min I = 2416250.889 + 32.31481d*E
(0 <= E <= 286, JD2416250 - 25482); Min I =
= 2416248.835 + 32.32145d*E (331 <= E <= 554, JD
2426940 - 34155); Min I = 2416244.990 +
+ 32.32765d*E (734 <= E <= 876, JD2439970 - 44570).
Brightness of the system out of eclipses periodi -
cally varies within 8.6m - 9.0m with elements
Max = 2416198 + 516.06d*E [5036]. Max - Min =
= 233d = 0.45P [0881]. Strong
emissions of H, NV, CIV, SIIV, FeIII.
Powerful gaseous stream and accretion
phenomena are possible.
RY Cas [A/H] = 0.0.
RZ Cas Min II 6.26. The light cur-
ve shape var; d var (0.000P <= d <= 0.009P). P var,
P var, variations are irregular. Mean
elements based on visual and photographic obser-
vations: Min I = 2416886.8806 + 1.195253065d*E
(JD2416800 - 26700) [8820], Min I = 2432820.7853 +
+ 1.1952517d*E (JD2426700 - 34000) [0938].
From photo-
electric observations: Min I = 2432115.5827 +
+ 1.1952472d*E (JD2429870 - 30400); Min I =
= 2432085.7011 + 1.195259d*E (JD2432000 -
- 32460); Min I = 2434349.5130 + 1.1952525d*E
(JD2432450 - 34420); Min I = 2434703.3035 +
+ 1.195238d*E (JD2434420 - 34705); Min I =
= 2435934.4087 + 1.1952499*E (JD2434705 -
- 35950); Min I = 2438829.2818 + 1.195243d*E
(JD2436800 - 39100); Min I = 2440182.3089 +
+ 1.195259d*E (JD2439380 - 40200); Min I =
= 2441333.3257 + 1.195244d*E (JD2440500 -
- 41350); Min I = 2442327.7798 + 1.1952521d*E
(JD2441550 - 42350); since JD2442850 -
- see Table.
SU Cas [A/H] = - 0.1.
SV Cas P var. Max = 2421839 + 279.3d*E (JD2417600 -
- 21900); Max = 2430450 + 281.7d*E (JD2422500 -
- 31900); since JD2432600 -
see Table.
SX Cas VB A (B 11.5m, 19", 250deg, 1966). Min II 9.32.
The light curve shape var.
DII = 0.171P:, dI = 0.036P, dII = 0.050P. P var.
Min I = 2433963.267 + 36.56727d*E (JD2418000 -
- 37000); since JD2438700 -
see Table. Strong emissions
of H, NV, CIV, SIIV, FeIII. Gaseous streams and accre-
tion phenomena.
SY Cas VB? P var. Max = 2417911.547 + 4.070969d*E (JD
2417000 - 34000); since JD2434000 -
See Table.
SZ Cas P var. Max = 2421261.66 + 13.6009d*E (JD2416700 -
- 21260); Max = 2426650.20 + 13.6072d*E (JD
2421260 - 27170) [8821]; Max = 2429727.240 +
+ 13.61744d*E (JD2427170 - 33050); Max =
= 2436810.92 + 13.62655d*E (JD2433050 - 38720);
since JD2438720 - see Table.
[A/H] = - 0.6.
TU Cas Fundamental mode period P0 is
given in the Table; the corresponding amplitude
is 0.69m. First-overtone period P1 = 1.51830d; the
corresponding mean amplitude decreased from
0.4m to 0.25m during 67 years [5078]. P1/P0 = 0.71.
M - m var (0.17P <= M - m <= 0.35P).
TV Cas d = 0.01P. Min II 7.34. The
light curve shape var.
Period of these variations - 600d [8822]. P var.
Mean elements
based on visual and photographic observations:
Min I = 2432827.7665 + 1.81260983d*E (JD2415650 -
- 32800) [1926].
From photoelectric observations Min I =
= 2432827.7665 + 1.8126142d*E (JD2432800 -
- 36490); Min I = 2436483.8091 + 1.81255d*E (JD
2436480 - 36980); Min I = 2438472.2386 + 1.81263d*E
(JD2437000 - 38500); Min I = 2438829.3230 +
+ 1.8126048d*E (JD2438470 - 41750); since
JD2441750 - see Table.
TW Cas Min II 8.40.
TX Cas Min II 9.6.
TY Cas P var. Max = 2419260 + 545.0d*E (JD2419200 - 25300);
Max = 2428965 + 623.8d*E (JD2427000 - 41500);
since JD2441500 - See Table.
UU Cas Min II 10.5.
UZ Cas [A/H] = -0.3.
VV Cas P var. Max = 2422514.16 + 6.207510d*E (JD
2417000 - 32500); since JD2432500 -
see Table. [A/H] = -0.2.
VW Cas [A/H] = 0.0.
WY Cas In the region of the cluster
NGC 7789.
The spectrum of
the G type star is seen in minimum light [3502]. The
existence of a physical companion is possible. S 6/6-e.
WZ Cas VB A (optical companion
B 8.7m, 58", 89deg). SC 7/10e.
Light variations
are sometimes taking place with doubled period.
XX Cas Min II 10.2.
YZ Cas VB A (B 11.23m, 35", 160deg). d = 0.045P. Min II 5.78.
ZZ Cas Min II 10.9.
AB Cas EA/SD. Min II 10.28. P var. Min I = 2430755.678 +
+ 1.366863d*E (JD2425400 - 33150); Min I =
= 2433616.532 + 1.366876d*E (JD2433150 - 37000);
Min I = 2440475.5216 + 1.3668783d*E (JD2437000 -
- 41600); since JD2441600 -
see Table.
The A3 component is a
DSCT type variable with the elements: Max hel =
= 2444912.1759 + 0.0582874d*E [8825];
amplitude of pulsations delta(V) var
(0.03m <= delta(V) <= 0.09m).
AE Cas Min II 12.8.
AH Cas Min II 13.3.
AL Cas Min II 13.6.
AO Cas Min II 6.24. The light cur-
ve shape var. P var?
AQ Cas Min II 10.4.
AR Cas VB A (B 9.3m, 1.0", 336deg; C 8.2m, 75", 269deg;
D 9.8m, 76", 268deg; E 11.28m, 43", 115deg; F 11.06m, 69",
338deg; G 11.11m, 67", 348deg). Min II 4.86; Min II - Min I =
= 0.614P; DII = 0.076P; dII = 0.037P.
AS Cas VB A (B 15.5m, 3", 45deg).
Fundamental mode pe-
riod P0 is given in the Table; the corresponding
amplitude is 0.59m. First-overtone period P1 =
= 2.2909d; amplitude of oscillations with this pe-
riod is 0.13m. P1/P0 = 0.76.
AX Cas Min II 12.9.
AZ Cas B - V: +1.78, +2.20. D = 110d, d = 88d = 0.026P.
BD Cas B - V: +1.50, + 1.61. P var. Max = 2429124.84 +
+ 3.65129d*E (JD2415000 - 29130) [0915];
since JD2429130 - see Table.
BE Cas VB A (B G, 25", 260deg).
BH Cas According to
[0453] tHere are no variable stars on the place of
BH Cas and in its surroundings.
BM Cas Min II 8.98.
Shape of the light curve varies. P var.
There is a perio-
dic term in the elements: + 2.6d sin (7.11deg*E + 104deg).
According
to [0939] on the light curve cepheid-like variati -
ons are observed with P = 27d.
BN Cas Min II 13.4.
BS Cas Min II 12.6.
BU Cas D = 0.02P.
BY Cas In the region of the cluster
NGC 663. P var. Max = 2416871.91 + 3.2218d*E (JD
2416800 - 24860) [0921]; Max = 2431929.60 +
+ 3.221297d*E (JD2426900 - 34300); Max =
= 2438399.629 + 3.222588d*E (JD2436200 - 39400);
since JD2439400 - see Table.
BZ Cas Min II 11.5.
CC Cas Min II 7.26. The light cur-
ve shape var? P var?
CE Casa Possible
member of the cluster NGC 7790. VB A (B =
= CEb Cas, 2.4", 265deg).
CE Casb VB B (A = CEa Cas). See CEa Cas.
of the cluster NGC 7790. [A/H] = 0.1.
CG Cas In the region of the cluster
NGC 7790.
CH Cas [A/H] = - 0.5.
CQ Cas The slow
oscillations are superimposed by more rapid ones
with cycles from 110d to 250d.
CR Cas Min II 13.3.
CS Cas [A/H] = - 0.4.
CV Cas Epochs given in [0922]
are not represented by the elements given in the
Table. P var?
CW Cas Min II 11.47.
Shape of the light curve
and depths of minima vary. P var. Min I =
= 2435745.6163 + 0.31886497d*E (JD2432400 -
- 41000) [3332]; since JD2441000 -
see Table.
CY Cas [A/H] = - 0.7.
DD Cas P var. Max = 2415612.45 + 9.807272d*E (JD
2415600 - 18600); since JD2418600 -
see Table. The star may be a
member of a binary system with Porb = 8500d +-
+- 1000d.
DF Cas In the region of the cluster
NGC 1027.
DI Cas P var. Max = 2432068 + 371.7d*E (JD2417200 -
32100); since JD2432100 -
see Table.
DL Cas Member of the cluster NGC 129.
[A/H] = 0.0.
DN Cas Min II 10.13.
DO Cas Min II 8.61; dI = 0.08P.
DP Cas Min II 13.6.
DZ Cas Min II 12.0.
EG Cas Min II 13.1.
EK Cas Depth of Min II 0.05m.
EM Cas P var. Max = 2433132 + 283d*E (JD2427700 -
33150); since JD2433150 -
See Table. Amplitude strongly varies.
EN Cas Min II 12.4. P var.
EP Cas Min II 11.4.
EQ Cas Min II 12.7. P var. Min I = 2432150.04 + 58.26d*E
(JD2432200 - 34060) [3336]; since JD
2436100 - see Table.
EY Cas Min II 14.5.
GG Cas d = 0.013P. Min II 9.99. P var? Min I = 2430188.468 +
+ 3.758738d*E (JD2424800 - 39500) [0936];
since JD2439500 - see Table.
GK Cas Depth of Min II 0.05m.
GT Cas d = 0.02P.
GU Cas Min II 11.3. P var. Min I = 2428749.423 +
+ 3.093329d*E (JD2417470 - 35480) [0941];
Min I = 2437367.375 + 3.09325d*E (JD2435480 -
- 38750) [0001]; since JD2438750 -
see Table.
GZ Cas Mean magnitude varies with P = 800d. Max =
= 2428000 + 800d*E [0911].
HH Cas Epoch of Min is given. RV type is possible
[0911].
HN Cas d = 0.038P.
HS Cas VB A (B 12m, 27", 15deg).
HT Cas Min hel = 2443727.93722 + 0.073647217d*E;
D = 0.13P. Depth of eclipses between outbursts
is ~ 2.4 V.
Small guasi-periodic
light oscillations with P = 100s.
Spectrum description [6163].
HU Cas P var. Max = 2417525.075 + 0.41159875d*E (JD
2411600 - 28000); since JD2428000 -
- see Table.
IL Cas Depth of Min II 0.05m.
IR Cas Min II 11.5. P var. Min I = 2428750.2914 +
+ 0.68069178d*E (JD2417500 - 38400) [0098];
since JD2438400 - see Table.
IS Cas Min II 12.2. P var. Min I = 2428776.262 +
+ 1.8415172d*E (JD2417400 - 29500) [0098];
since JD2428000 - see Table.
IT Cas Min II 11.8; Min II - Min I = 0.553P; DII = 0.042P.
Apsidal motion is possible.
IV Cas Min II 11.3. P var. Min I = 2428991.302 +
+ 0.9985232d*E (JD2416700 - 29000) [0098];
Min I = 2431438.648 + 0.9985056d*E (JD2429000 -
- 37700) [2263]; since JD2440000 - see Table.
IW Cas S 4 + /6 e.
IX Cas P var. Max = 2428749.39 + 9.15035d*E (JD2414700 -
- 29500) [0098]; Max = 2428749.90 + 9.1363d*E
(JD2428700 - 34350) [0944]; Max = 2437195.642 +
+ 9.14783d*E (JD2434350 - 39100) [5462];
since JD2442000 - see Table.
[A/H] = -0.4.
KL Cas Min II 12.3.
KO Cas P var. Max = 2425590 + 305.6d*E (JD2416700 -
- 26000); since JD2426000 - see Table.
KR Cas Min II 9.9.
LR Cas Min II 10.9.
Lu Cas Min II 14.3?
LW Cas In the apex of A small (8") bright co-
metary nebula in the region of IC 1848. Novali-
ke outburst was observed in the interval JD
2433900 - 34800.
Infrared and radioemission.
LX Cas In the region of the cluster
Collinder 33. Min II 15.3; Min II - Min I = 0.47P;
dI = 0.10P.
LY Cas In the region of the cluster
Collinder 33. Min II 15.2.
MM Cas d = 0.08P: Min II 12.4.
MN Cas Min II 10.57.
MO Cas In the nebula NGC 7635.
10.2 - 13.1 I.
MP Cas In the nebula NGC 7635.
10.4 - 13.5 I.
MR Cas Min II 15.5.
MS Cas Min II 13.2.
MT Cas d = 0.04P. Min II 14.02.
MU Cas Min II 10.8.
MV Cas Min II 14.0.
MY Cas Min II 15.2. P var.
Elements given in the Table are valid
since JD2438500.
NN Cas Min II 14.0.
NT Cas Min II 14.4.
NU Cas Min II 13.4.
NV Cas d = 0.03P.
OP Cas P var. Max = 2429109.726 + 5.510019d*E (JD
2427950 - 34670) [0176]; since JD
2437000 - see Table.
OR Cas Min II 11.8. P var. Min I = 2429249.424 +
+ 1.2457026d*E (JD2413800 - 34800) [0176];
since JD2432000 - see Table.
OX Cas In the region of the cluster
NGC 381. d = 0.016P. Min II 10.30; Min II - Min I =
= 0.512P. Apsidal motion [4524].
PR Cas P = 171d?
PV Cas Min II 10.36; Min II - Min I = 0.480P.
Depth of Minima probably varies. P var. Min I =
2428796.8142 + 1.75047346d*E (JD2415700 - 40000) [5302];
since JD2440000 - see Table.
Apsidal motion
[6253]: Min II = 2428797.6894 + 1.75047346d*E -
- 0.040d sin 0.0075deg, (E - 3000).
PX Cas Min II 15.0.
PY Cas Epoch of Min brigh-
ness is given. Similar to RV Tau by light curve
shape [3348].
PZ Cas VB A (B 12.8m, WN 8:, 15", 100deg). OH, H2O
emission.
QQ Cas Min II 10.8. P var. Min I = 2434330.169 + 2.142030d*E
(JD2415700 - 30000) [2530]; since JD
2430000 - see Table.
QX Cas In the region of the cluster
NGC 7790. VB A (B 13.1m, 3"). Min II 10.50;
Min II - Min I = 0.37P; DII = 0.047P; dII = 0.018P.
V 336 Cas Min II 13.6.
V 341 Cas d = 0.031P.
V 344 Cas Min II 13.4.
V 345 Cas Min II 13.6.
V 357 Cas Min II 13.6.
V 359 Cas Min II 12.0.
V 360 Cas Min II 12.3.
V 361 Cas d = 0.051P.
V 363 Cas delta(S) = 1.
V 364 Cas Min II 11.9.
V 365 Cas S 6/3 - .
V 366 Cas Min II 12.7. P var. Min I = 2435075.461 +
0.7292714P*E (JD2414600 - 35400) [2305];
since JD2434650 - see
Table.
V 373 Cas An unique
close binary. Porb = 13.4192d [4627]. Epoch
of Min I is given close to the epoch of one
of conjunctions. Min II - Min I = 0.58P. Maxima
are very sharp. Max - Min II = 0.25P. It is not
excluded that the star is an eclipsing one
with physical variability of components, but
eclipses, if they exist, cause only a very
small part of the observed light variations.
Range of light variations is given according
to [2651]. As a rule the amplitude is close to
0.1m.
V 374 Cas Min II 12.1.
V 375 Cas Min II 10.6.
V 377 Cas VB (A 8.5m; B 9.4m, 2.1", 185deg, 1962).It is
not known which component varies.
According to [4005] the range
of combined brightness variations is 0.26m.
According to [7051], const.
V 380 Cas d = 0.08P.
V 381 Cas Min II 10.8.
V 388 Cas Wolf 47 (mu = 0.82", p = 80deg).
Faint component of a wide phy-
sical pair (p = 294") the bright component of
wich is the dM2 star Wolf 46 = BD +61deg 195 (9.4).
V 392 Cas Min II 14.0. P var. Min I = 2429640.390 +
+ 4.54094d*E (JD2425300 - 29640); Min I =
= 2429640.390 + 4.54064d*E (JD2429640 -
- 36900) [4027]; since JD2436900 -
see Table. Depth of Min
var?
V 394 Cas Min II 15.6.
V 396 Cas Min II 10.2.
V 399 Cas Min II 14.1.
V 401 Cas Min II 15.7.
V 402 Cas Min II 15.3.
V 406 Cas Min II 16.8.
V 410 Cas Bright in 1938 -39. Slow. Not red.
V 423 Cas Min II 14.3.
V 427 Cas Min II 13.7.
V 428 Cas Red.
V 430 Cas NortHern component of a close pair. Red.
V 434 Cas Red.
V 441 Cas P = 351.2d?
V 442 Cas d = 0.025P. P var? Since 1972
P = 3.592120d.
V 444 Cas Min II 16.0. P var. Min I = 2438651.314 +
+ 2.224808d*E (JD2432850 - 37300);
since JD2437300 - see Table.
Period variation may be cyclic.
Mean elements: Min I = 2443194.258 +
+ 2.224773d*E.
V 445 Cas Min II 11.08.
V 448 Cas Min II 15.0.
V 450 Cas VB A (B 17.5m:, 3.4", 188deg).
Range
of combined light variations is given.
V 459 Cas Min II 11.6.
V 466 Cas In the region of the clus-
ter NGC 457.
V 480 Cas Min II 14.7.
V 482 Cas VB A (B 10.0m, F 4 V, 6", 195deg;
optical). P = 0.28292d?
V 497 Cas In the region of the clus-
ter IC 1848.
V 498 Cas See V 497 Cas.
V 499 Cas See V 497 Cas.
V 509 Cas Pulsation of photosphere with P = 3 years.
Tenuous shell ejected in 1975 is now falling back to
the star.
V 518 Cas In the region of the clus-
ter Stock 2. Star N136 (Stock 208).
V 520 Cas Min II 13.1. P var. Min I = 2439069.559 +
+ 0.489832d*E (JD2438580 - 40850);
since JD2441150 - see Table.
V 521 Cas Member of the cluster NGC
7789.
V 523 Cas Min II 11.34. P var. Min I = 2432054.555 +
+ 0.2336882d*E (JD2428545 - 33570) [7008];
Min I = 2439029.461 + 0.23368912d*E (JD
2439000 - 41300) [7387]; since JD
2440480 - see Table.
V 524 Cas OH, H2O emission. P = 163d?, 191d?
259d?, 620d?
V 526 Cas Two oscillations are superimposed: P1 = 0.0526d (A1 =
= 0.0036m), P2 = 0.0396d (A2 = 0.0056m); P2/P1 =
= 0.753.
V 527 Cas Min II 13.5; Min II - Min I = 0.52P.
V 532 Cas - V 533 Cas
In the region of the cluster NGC 7789.
V 536 Cas P var. Max = 2438700.262 + 0.395674d*E (JD
2438580 - 39150); Max = 2441186.333 +
+ 0.395683D*E (JD2440070 - 41250);
since JD2441500 - see Table.
V 540 Cas Epoch of Max (U) is given.
V 541 Cas Min II 11.0.
V 542 Cas See V 532 Cas.
V 544 Cas Elements given in the
Table are valid since JD2428000.
V 546 Cas In the region of the clus-
ter NGC 103. Min II 14.8.
V 547 Cas VB A (B 12.4m, M 4.5, 2.8", 93deg).
Astrometric binary (A = 0.12",
P = 15.9A); mu = 1.75", P = 98deg.
Variation of
combined light is given.
V 551 Cas P = 45.5d?/57d.?/67.5d?.
V 554 Cas P >= 3500d? D = 400d?
V 559 Cas VB A (B 7.7m, 0.25", 34deg, 1976). Min II 7.21.
V 566 Cas VB A (B 8.3m, 1.4", 194deg, 1965).
V 569 Cas 10.0 - 14.7 I.
V 589 Cas In the cluster NGC 663.
V 592 Cas White dwarf. Rapid non-perio-
dic fluctuations of brightness on a time scale
of several minutes.
V 598 Cas VB A (B 12m, 19", 0deg). P = 2.825d? [2560].
V 615 Cas Variable radio source on 10.5
GHz; gamma - and X-ray source?
V 627 Cas H2O emission.
V 635 Cas 4U 0115 + 634.SB (P = 24.3162d).
Pulsar period P = 3.6136s.
V 638 Cas Epoch of Min is given.
alf Cas VB A (B 14.5m, 17.6", 272deg; C 13.5m, 38", 105deg;
D 8.5m, 64.4", 280deg.
bet Cas VB A (B 13.7m, 31.3", 243deg); SB (P = 27d).
[Fe/H] = 0.64.
gam Cas VB A (B 11.0m, 2.2", 248deg; C 13.0m, 52.2", 348deg).
In HII region S 185.
X - ray source MX 0053 + 60. V sin I = 310 km/s.
del Cas VB A (B 11.5m, 31.7", 66deg). Min II 2.75. Min II - Min I =
= 361d.
The elements given in the Table
are still not confirmed by anyone.
iot Cas VB A (B 6.89m, 2.3", 239deg; C 8.40m, 7.2", 114deg).
Astrometric binary
(A = 0.113", P = 52.4A). Max (V) - Max (lambda 1550) = 0.4P;
A (lambda 1550) = 0.40m.
The range
of total brightness variation of components A and
B is given.
kap Cas P = 0.09028D, P (Vr) = 0.14035d [2588]; P = 7d [8876].
omi Cas VB A (B 11.7m, 33.6", 303deg). SB 1 (P = 1033d);
V sin I = 220 km/s.
ro Cas Usually varies within the limits 4.4m - 5.2m V.
In november 1945 the peculiar decrease of bright-
ness began lasting for 165d and in September
1946 the star reached the middle of the deepest
Minimum (JD2432070) lasting for 320d. Then
the brightness began to increase symmetrically
and July 1947 the star attained its normal bright -
ness [0957]. Photographic magnitudes varied in
the limits 5.4m - 8.3m. Spectrum description [8878].
B Cas Tycho Brahe's superno-
va. Stellar object is not identified
optically up to now.
R Cen VB A (B 12m, 28", 218deg). Epoch
of Min I is given. Min I 0.00P, Max I 0.23P, Min II
0.47P, Max II 0.64P. 5.8, 6.0,
11.1, 8.3. P var. P = 561.3d
Before 1918; since 1918 - see
Table. H2O maser.
V Cen In the field
of the open cluster NGC 5662.
Z Cen SN 1895 (NGC 5253).
RR Cen Min II 7.63. dII = 0.08P. P var. Min I = 2424231.0910 +
+ 0.60568807d*E + 2.31d*10**-10*E**2 (JD2414170 -
- 33470) [0006]. Current elements - see Table.
RS Cen A 1118 - 61?
RT Cen P var.
RZ Cen Min II 9.4.
SS Cen Min II 9.5.
ST Cen Min II 11.30, DII = 0.22P. Max II (before
Min I) 10.65.
SU Cen Min II 9.2.
SV Cen Min II 9.45. delta(m) var. P var. Min = 2433053.358 +
+ 1.6594795d*E - 7.61d*10**-8*E**2 (JD2412608 -
- 42097).
Cyclic (32a - 33.6a) pe-
riod variations were noted in [0009, 5212].
since 1978 - see Table.
P Cyg profiles in the spec-
trum.
SX Cen For mean light Max =
= 2426835 + 615d*E.
SY Cen d = 0.05P.
SZ Cen VB. Min II 8.7.
TX Cen VB? B - V: +1.39, +2.11.
TZ Cen The co-ordinates in the Table are based on
[0015]. According to [0016], no star brighter
than 14m was found in this position. The co-ordi-
nates in [0015] may be in error.
UW Cen IR excess.In Max varies se-
miregularly, P ~ 42d [8832].
UZ Cen VB A (B 13.8m, 4", 191deg). Max II = 2440746.2 +
+ 2.35529d*E.
VW Cen VB A (B ~ 15m?, ~ 8", ~ 180deg). B - V: +1.01, +1.71.
[A/H] = 0.3.
VZ Cen Min II 8.4.
WX Cen ~ + 0.45, ~ - 0.72.
Proposed as an optical
counterpart of the transient X-ray source
Cen X - 2 [5314], Though no optical bursts were
observed.
WZ Cen Min II 14.2.
ZZ Cen VB C (A 9.4m, B9; B 10.8m, 8", 314deg; C = ZZ Cen,
9", 259deg; D = AA Cen, 9", 110deg).
AA Cen VB D (See ZZ Cen).
AB Cen d = 0.05P.
AP Cen Epoch of Min is given.
AS Cen Min II 13.2.
AV Cen Min II 14.1.
AZ Cen The shape of
the light curve varies.
BD Cen Min II 10.7.
BF Cen In the field
of the open cluster NGC 3766. Min II 8.8.
BG Cen Min II 12.3.
BH Cen In the open cluster
IC 2994. Min II 8.8.
BI Cen delta(S) = 2.
BK Cen P2 = 2.236d, A1 = 0.54m, A2 = 0.22m [8835].
BV Cen The mean cyc-
le between outbursts <= 149.4d [7301]. The tabula-
ted elements correspond to Max of the eclipsing
light curve, fi (Min) = 0.25P. The range of the eclip-
sing variability is 12.8 - 13.3.
CN Cen Min II 13.3.
DI Cen Min II 12.3, Min II - Min I = 0.494P, DII = 0.08P:.
DT Cen Red.
DX Cen The P star in a pair.
DY Cen All spectral lines
are very weak. No IR excess. The photometric
behaviour outside major Min of described in
[8836].
EP Cen Min II 11.5.
EU Cen See DX Cen.
GI Cen In the field of
the globular cluster NGC 5286.
IQ Cen d = 0.04P.
IW Cen Min II 12.1.
IX Cen In the field
of the open cluster NGC 3706.
IY Cen In the field
of the open cluster IC 2944.
IZ Cen = 1.7.
KK Cen B - V: +1.08, +1.62.
KM Cen Min II 13.3.
KN Cen B - V: +1.36, +1.75. [A/H] = 0.2.
KQ Cen Alternating periods 136d, 159d.
KT Cen B - V: +0.46. Min II 12.72. Min II - Min I = 0.392P
(JD2441686 - 721);
Apsidal motion is observed [8094].
KY Cen Min II 13.3.
KZ Cen B - V: +0.30, +0.72.
LL Cen Min II 13.1.
LR Cen Min II 12.30.
LT Cen Min II 9.6.
Lu Cen The period may be twice longer.
LV Cen B - V: +1.3, +1.7.
LW Cen Min II 9.6. See IY Cen.
LX Cen Min II 13.55.
LZ Cen Min II 8.50.
MM Cen Min II 12.7.
MN Cen Min II 8.7. VB A (B 10.9m, 7", 147deg).
MP Cen Min II 10.0.
MQ Cen Min II 10.1.
MR Cen Min II 10.5.
MV Cen Min II 14.6.
MY Cen B - V: +1.58, +1.94.
NO Cen Min II 14.2.
NP Cen Min II 10.2.
NY Cen Min II 11.9.
OO Cen = 1.84.
OP Cen Min II 13.8.
OU Cen Min II 10.9.
OV Cen Min II 11.0.
OX Cen Min II 14.3.
QS Cen d = 0.03P.
QT Cen Min II 13.4.
QY Cen = 2.16.
QZ Cen P var? The shape of the light curve varies?
V 339 Cen VB A (B ~ 13m, SP). B - V: +1.08, +1.47.
V 343 Cen Min II 13.5.
V 344 Cen Min II 12.3.
V 346 Cen In the field of the open cluster Stock 14. Min II 8.8.
Min II = 2421966.835 + 6.32189d*E.
V 348 Cen d = 0.010P.
V 349 Cen Min II 14.5.
V 350 Cen Min II 10.3. Min II = 2430870.192 + 3.216906d*E.
V 351 Cen See AP Cen.
V 356 Cen Min II 15.0.
V 358 Cen See AP Cen.
V 365 Cen d = 0.040P.
V 373 Cen VB A (B ~ 4" np).
V 377 Cen d = 0.003P.
V 379 Cen Min II 8.9.
V 380 Cen Min II 10.0.
V 383 Cen Min II 13.6:, Min II - Min I = 0.609P.
V 384 Cen Min II 12.2. DII = 0.062P. Min II - Min I = 0.667P.
V 385 Cen Min II 13.0.
V 388 Cen Min II 15.7.
V 399 Cen d = 0.020P. Min II 13.1.
V 405 Cen P var, 30d - 40d.
V 412 Cen VB A (B 59", 266deg).
V 419 Cen P var. Max = 2428099.25 + 5.50713d*E
(JD2428099 - 33573); since
JD2434900 - see Table.
V 420 Cen B - V: +0.45, +0.97. P var.
Nonlinear term: -0.000090d*E**2.
V 427 Cen Epoch of Min is given.
V 436 Cen SB (P = 0.0669d). Photometric P during super-
maxima 0.06383d [8838]. Rapid oscillations in super -
maxima delta(m) ~ 0.002m, P ~ 19.6s [8049].
V 440 Cen d = 0.033P. Min II is possible.
V 443 Cen d = 0.025P.
V 491 Cen Very flat minima; close companion?
V 495 Cen d = 0.042P. Min II 10.6. Min II - Min I = 0.520P.
V 496 Cen Possible member of the open cluster NGC 4755.
B - V: +1.02, +1.33.
V 498 Cen P may be twice shorter.
V 499 Cen (k - b)2 = 0.23.
V 504 Cen Semiregular variations (P1 ~ 130d, P2 ~ 411d)
are also observed [8836].
V 508 Cen Min II 13.2.
V 526 Cen delta(m) var. P var. Max = 2425707.540 + 0.56153d*E
(1929 - 1930); during 1931 - 1940
- see Table.
V 532 Cen Star 1 [9078]. X-ray source
3A 1431 - 409.
V 544 Cen 2AS E 1440 - 39? [5962].
V 545 Cen Magnitude in Max var (12.6 -
- 14.5), P = 1800d?
V 553 Cen [Fe/H] = -0.1; [C/Fe] = +0.8.
V 565 Cen Min II 13.9. Type RR is not excluded (P = 0.238072d).
V 574 Cen sp star of a pair.
V 585 Cen Min II 13.0.
V 592 Cen Mean brightness var.
V 593 Cen Possible member of the open cluster Stock 16.
Min II 11.2.
V 594 Cen V 133 (omega Cen); non-mem-
ber of the cluster. Min II 14.4.
V 606 Cen Min II 9.8.
V 607 Cen Min II 14.1.
V 608 Cen Min II 13.1.
V 609 Cen Min II 13.6.
V 615 Cen Min II 14.0.
V 617 Cen Min II 13.8:.
V 619 Cen In the field of the open cluster NGC 5316.
V 621 Cen d = 0.05P.
V 624 Cen Min II 14.9.
V 625 Cen Min II 15.0.
V 627 Cen d = 0.02P.
V 628 Cen Min II 13.2.
V 630 Cen Min II 14.2. d = 0.06P.
V 635 Cen Min II 13.9.
V 636 Cen Min II 8.8.
V 644 Cen During the faint phase in 1951 the
shell spectrum was observed [2128]. Type E
with a very long period is possible [6763].
V 645 Cen Proxima Cen = alfa Cen C. mu = 3.809", P = 281.7deg.
Soft X-ray source.
V 646 Cen d = 0.022P. Min II 9.1.
V 662 Cen P ~ 2.48d or 2.95d.
V 672 Cen Min II 11.4 - 11.6 (var).
V 673 Cen Depth of Min II 0.05m.
V 674 Cen Blazhko effect: Pi = 29.5d.
0.15P <= M - m <= 0.23P.
V 676 Cen Min II 12.5.
V 677 Cen Min II 11.6.
V 678 Cen Min II 10.6.
V 679 Cen 9.8"p, 1.1"n from CPD - 62deg 2167.
The star is at the edge of a dark cloud in a
bright nebula, a part of IC 2944, in the field
of a very poor open cluster. Since 1950 till
1954 faded by 2.5m. Rather red. "Screening"
by the edge of a dark nebula?
V 682 Cen IR excess.
V 684 Cen Depth of Min II 0.05m.
V 685 Cen Min II 9.5.
V 686 Cen RV type is not excluded.
V 687 Cen Min II 14.1. DII = 0.12P. Min II - Min I = 0.580P.
V 688 Cen Min II 12.7.
V 689 Cen Min II 12.1.
V 690 Cen Depth of Min II 0.03m.
V 692 Cen Min II 11.6. Min II - Min I = 0.481P.
V 701 Cen VB? d = 0.026P. Min II 9.1.
V 704 Cen IR excess.
V 716 Cen Min II 6.21.
V 742 Cen Min II 10.1.
V 743 Cen (k - b)2 = 0.20.
Element almost as well satisfactory: Max =
= 2439243.6465 + 0.10222560d*E.
V 745 Cen Min II 9.6.
V 746 Cen = V 467 Cen.
V 467 Cen. Marked as V 467 cen in the chart.
V 747 Cen Min II 10.05.
V 748 Cen B - V: +0.31, +1.21; U - B: -0.66, -0.21. d =
= 0.106P. Narrow halfa emission. Outside eclipses shows
variations by 0.05m - 0.1m during several days or se-
veral weeks (probably irregularly) [6968].
V 752 Cen Min II 9.61. dI = dII = 0.047P.
V 753 Cen (k - b)2 = 0.20.
In the field of the open
cluster NGC 3960; probably nonmember. Type
DSCT is possible.
V 754 Cen Slight Min II.
V 755 Cen In the coalsack.
V 756 Cen See V 755 Cen.
High excitation lines (OVII,
OVIII, CV) are present in the spectrum. WR
type is possible [7372].
V 757 Cen Min II 8.6.
V 758 Cen d = 0.07P. Min II 9.15.
V 759 Cen Min II 7.56.
V 761 Cen IR excess.
V 763 Cen VB A (B 13m, 7", 163deg).
V 766 Cen VB A (B 10.01m, BOIbp, 9", 318deg).
IR excess.
V 767 Cen VB A (B 11.52m, 21", 350deg).
V 768 Cen Possible P: 60d - 80d.
V 770 Cen According to [7570], const?
V 772 Cen In the region of the open cluster IC 2944.
V 775 Cen EB type is possible. Deep Min II.
V 777 Cen Deep Min II.
V 779 Cen Cen X-3 (3U 1118 - 60). : +1.04;
: -0.08. Min II 13.39. Porb var.
The shape of the
light curve varies. Epoch of Min I is given.
Epochs of Min II coincide with the moments of
X-ray eclipses. X-ray pulses are observed
with Ppuls = 4.834477s (epoch JD2442785.3);
Ppuls decreases [7612]. No rapid optical os -
cillations were found.
V 783 Cen B - V: +0.35.
V 784 Cen Very red.
V 788 Cen Min II 5.90.
V 790 Cen VB B (A 4.52m; 60", 343deg).
V 791 Cen In the region
of globular cluster omega Cen (NGC 5139).
Cluster non-member.
V 795 Cen VB A (B 12.29m, 33.9", 170deg; C 12.79m, 36",
220deg).
V 801 Cen 4U 1145 - 61 = 2S 1145 - 619.
Primary component has a low density envelope ex-
panding with the velocity of 1800 km/s.
V sin i = 290 km/s. X-ray pulsar (P = 291.8s
[8883]). Max (X) = 2442519.5 + 187.5d*E [8881].
V 803 Cen Extremely hot hydrogen-deficient helium star.
V 807 Cen VB (9.9m, 10.1m, 0.4", 258deg, 1931).
It is not known which of the components varies.
V 810 Cen Member of the cluster Stock 14.
V 813 Cen See V 791 Cen. V 65 (NGC 5139).
V 814 Cen See V 791 Cen. V 78 (NGC 5139).
Min II 14.165:. Primary component
is probably intrinsically variable [8884].
V 816 Cen Primary oscillation is superim-
posed by the oscillations with freguencies:
F2 = 4.9229, F3 = 4.7343, F4 = 4.9317 [2591].
V 820 Cen [Fe/H] = -2.5; Vr = +260 km/s.
V 822 Cen Cen X-4.
V 825 Cen See V 791 Cen. V 2 (NGC 5139).
V 826 Cen See V 791 Cen. V 129 (NGC 5139).
bet Cen VB A (B 4.1m, 1.3", 251deg, 1960). SB 1 (P = 352d
[8887]. Multiperiodicity; sometimes
brightness is constant [8215].
Soft X-ray source.
del Cen VB A (B 4.8m, 68.6", 325deg; C 6.5m, 16.6", 227deg).
eps Cen VB A (B 13.0m, 36.0", 158deg).
THere is a secondary light oscillation with
the amplitude of 0.0034m and elements: Max =
= 2441041.058 + 0.17696d*E.
eta Cen VB A (B 13.5m, 5.6", 270deg, 1897); SB?
mu Cen VB A (B 13.63m, 48", 128deg).
omi 1 Cen
VB A (B 11.4m, 13.5", 125deg).
T Cep P var. Max = 2414252 + 386.05d*E (JD2406900 -
- 20490); Max = 2431086 + 394.93d*E (JD2420490 -
- 32900); Max = 2440262 + 379.22d*E (JD2432900 -
- 42200); since JD2442200 Max = 2444171 +
+ 392.7d*E. Mean value of the period is given in
the Table. SiO maser.
U Cep VB A (B 11.83m, 13.9", 62deg; C 12.3m, 23.0", 318deg).
0.010P <= d <= 0.040P. Min II 6.93. P var. Min I =
= 2407890.3346 + 2.4928551d*E + 5.15d*10**-9*E**2
(JD2388855 - 2440790) [6468];
Analysis of period variations in this in-
terval see also in [7395]; Min I = 2441395.3604 +
+ 2.4931048d*E (JD2440790 - 41600); Min I =
= 2441679.5716 + 2.4930432d*E (JD2441600 - 950);
Min I = 2443753.7982 + 2.4930679d*E (JD2442100 -
- 43800); since JD2444000 -
see Table. Shape of the light curve
and depth of minima vary. Bright-
ness of the secondary (G8) varies sporadically.
Subgiant brightening accompanies eruptive mass
transfer. The gaseous stream moving to the pri-
mary (B7) component formes around it gaseous
ring or disc [8889].
W Cep SLow oscillations with Pi ~ 2000d are superimposed by os -
cillations with P ~ 350d.
X Cep OH emission?
RS Cep d = 0.039P. P var. Min = 2417140.469 + 12.419925d*E
(JD2410000 - 31000) [2431]; since JD
2431000 - see Table.
RZ Cep P var. Max = 2411640.654 + 0.308697d*E (JD
2411640 - 15000); Max = 2417144.620 + 0.3086203d*E
(JD2415600 - 20200); Max = 2421175.611 +
+ 0.3086699d*E (JD2421175 - 23000); Max =
= 2423768.475 + 0.3086918d*E (JD2423000 - 31700);
Max = 2433768.493 + 0.3086383d*E (JD2433700 -
- 38300) [8890]; Max = 2438207.938 + 0.308645d*E
(JD2438200 - 39040) [3879]; Max = 2440834.579 +
+ 0.3086735d*E (JD2440800 - 42640) [8890];
since JD2442640 - see Table.
Shape of the
light curve and the amplitude a vary with the
Blazhko effect period Pb = 96.8*P0 = 29.88d;
Min A = 2441464.147 + 29.88d*N [8891].
Long period variation of P0 with
a period ~ 50 years is possible. delta(S) = 6.
SS Cep Mean brightness va-
ries with cycles from some hundreds to thousands
days.
SU Cep Min II 10.6.
SV Cep IR excess.
SX Cep In the region of the nebula
NGC 7023.
SY Cep Min II 12.70. P var?
SZ Cep VB A (B 12.3m, 24.9", 263deg). S4/6 e.
TT Cep VB A (B 17.0m, 8", 160deg).
TY Cep Epoch of Min I is given.
UZ Cep P var. Max = 2440969 + 297.68d*E (JD2414000 -
42000); since JD2440000 -
see Table.
VV Cep VB (0.05", 174deg, 1950)? 0.066P <= D <= 0.091P;
0.040P <= d <= 0.077P. Depth of
eclipses: 2.30m (lambda 3500 A), 1.9m (U), 0.4m (B).
M - component is of
SRC type: Max = 2443045 + 118.37d*E [8698, 8894];
A(V) <= 0.33m.
Light oscillations are also noted with P ~
~ 58d [8895], 25d and 150d [8896].
B - component may be also an intrinsic variable [2416].
Gaseous streams. Strong variable magnetic field.
VW Cep VB A (B 10.3m, A = 0.51", P = 30.45a [8897]); mu alfa =
= +0.0899s, mu delta = + 0.560". Min II 7.56.
Shape of the light curve and depths of Min I and Min II
vary. P var. Min I = 2433483.4257 + 0.27831758d*E +
+ 0.050d*cos 0.004813deg*(E - 4700) (JD2424763 -
- 41200) [6483]; since JD2441000 -
See Table.
Period change study see also in
[8899]. X-ray source.
VZ Cep Min II 9.93.
WX Cep Min II 9.14; dI = 0.01P, dII = 0.00P.
WY Cep Min II 11.5. P var [2545].
WZ Cep Min II 11.9.
XX Cep Min II 9.26. P var. Min I = 2425096.449 + 2.337340d*E
(JD2414930 - 30000); Min I = 2441539.4917 +
+ 2.3373059d*E (JD2430000 - 42300) [8902].
since JD2441500 - see Table.
XY Cep Min II 10.10. P var?
XZ Cep Min II 8.43.
ZZ Cep VB A (B 10.2m, A2 P, 3.6", 202deg; C 10.87m, A5V,
20.6", 219deg). Min II 8.74.
AH Cep Min II 7.03. Depth
of minima varies. P var. Min I = 2434989.3702 +
+ 1.7747274d*E (JD2415500 - 35000) [3604];
since JD2434900 - see Tab-
le: + 3.12d*10**-9*E**2.
AI Cep Min II 9.48.
AN Cep Since JD2425200 primary and
secondary maxima and minima appeared, and
mean cycle became 254d.
AV Cep d <= 0.04P.
BB Cep d = 0.050P.
BE Cep Min II 13.0.
BF Cep P var. Max = 2437236 + 426.11d*E (JD2423600 -
37300); Max = 2441665 + 442.3d*E (JD2437300 -
42500); since JD2442500-
see Table.
BH Cep Sometimes strong Algol-like light weake-
nings are observed.
BO Cep See BH Cep.
CO Cep Min II 12.6; Min II - Min I = 0.552P; DII = 0.080P.
CP Cep P var?
CQ Cep Shape of the
light curve and depth of minima vary. According
to [7401] on 1969 March 28/29 on the phase
0.56P a light decrease by 0.1m was observed and
then a rapid flare by 0.35m U, 0.13m B, 0.14m V.
P var. Nonlinear term:
-10**-9*E**2.
CR Cep P var. Max = 2436846.94 + 6.23318d*E (JD2415000 -
- 30000) [3157]; since JD2430000 -
see Table.
CV Cep S7/1.5.
Mean brightness varies with a
cycle ~ 2000d [0159].
CW Cep VB A (B 12.29m, 20", 310deg). Min II 8.01; Min II -
- Min I = 0.478P (1972 yr).
There is a sinusoidal term
in the elements: + 0.0250d*sin (0.0626deg*E - 28.3deg).
Apsidal motion with P = 43a.
CX Cep Min II 12.16.
CY Cep Min II 16.5.
DD Cep P var. Max = 2427960 + 167.6d*E (JD2427900 -
- 30000); Max = 2429968 + 173.0d*E (JD2429900 -
- 33600); since JD2433600 - see Table.
DH Cep In the region of the cluster
NGC 7380.
Apsidal motion with P = 2.6a [0165].
DK Cep Min II 12.4.
DL Cep Min II 12.7.
DO Cep VB B (A 9.87m, M4V; A = 2", 4, P = 44.78a, E = 0.408);
mu = 0.852", P = 242.6deg.
DP Cep Min II 14.4.
DQ Cep Multiperiodicity: P0 =
= 0.12420d: [8137], P1 = 0.061177d [8914].
DX Cep P var. Max = 2430603.712 + 0.5260395d*E (JD
2415700 - 31000) [0001]; since JD
2431000 - see Table. delta(S) = 7.
DY Cep Min II 11.8.
EE Cep A var?
EF Cep Min II 12.6. P var?
EG Cep Min II 9.61. P var. Min I = 2439774.3322 +
+ 0.54462091d*E (JD2415200 - 41000) [0001];
since JD2441000 - see Table.
EH Cep In the dark cloud near the diffuse
nebula and the cluster NGC 7023.
EI Cep Min II 7.98.
EK Cep Min II 8.06; Min II - Min I = 0.545P (1965). Min II =
= 2439022.8484 + 4.427797d*E [8160].
Apsidal motion (P = 4700a +- 600a)
[8923].
EL Cep P var.
EM Cep In the region of the cluster
NGC 7160. VB A (A 12.8m, 19.8", 281deg; B 7.9m,
62.5", 146deg). Min II 7.16.
Shape of the
light curve and depth of minima vary.
EO Cep Min II 12.3.
EP Cep In the cluster NGC 188. Min II 17.0.
EQ Cep In the cluster NGC 188. Min II 16.7.
ER Cep In the cluster NGC 188. Min II 16.27.
ES Cep In the cluster NGC 188. Min II 15.8.
P var. Min I = 2439082.238 + 0.34468d*E (JD
2438480 - 39090); Min I = 2439236.501 + 0.34264d*E
(JD2439090 - 39280); Min I = 2439594.548 +
+ 0.34250d*E (JD2439400 - 39600); since
JD2439600 - see Table. A var.
EX Cep Min II 11.6.
EY Cep Min II 10.4.
EZ Cep P var. Max = 2416803.627 + 0.378990d*E (JD
2415400 - 20000) [0001]; since JD
2420000 - see Table.
FH Cep Min II 12.1.
FL Cep d = 0.02P.
FS Cep Min II 12.0.
FT Cep VB A (B 18.3m, 5", 27deg). See FU Cep.
FU Cep In the region of the diffuse nebula and the clus -
ter NGC 7023.
FV Cep See FU Cep.
The variable may be an eclipsing binary with
P = 0.4628d.
FW Cep See FU Cep.
GI Cep Min II 11.9.
GK Cep Min II 7.35; dI = dII = 0.03P; Min II - Min I = 0.502P.
P var. Min I = 2425189.526 + 0.9361614d*E (JD
2415000 - 27500); Min I = 2438694.7070 +
+ 0.9361714d*E (JD2427500 - 38200) [0001];
since JD2438200 - see Table.
GL Cep In the region of the diffuse nebula
IC 1396 and the cluster Tr 37.
GM Cep See GL Cep.
GP Cep In the region of the
HII zone S 132.
Quadruple sys-
tem, consisting of a WN6 + O8 - B0III: eclipsing
pair (P = 6.6883d) physically associated with an
O + O pair (P = 3.4698d); the latter pair may be also
an eclipsing or ellipsoidal variable [8931].
GS Cep Min II 10.6.
GT Cep Min II 8.6.
GW Cep Min II 12.00.
NK Cep Min II 14.4.
HZ Cep See FU Cep.
IL Cep VB A (B 11.91m, 7", 326deg); P = 2.802d?
IM Cep Min II 13.6.
IO Cep Min II 11.7.
IP Cep Min II 12.1.
IR Cep VB (delta(m) ~ 0.0m, 0.0" - 0.2"). P var. Max = 2431060.878 +
+ 2.114016d*E (JD2428335 - 31060) [0001];
since JD2440900 - see Table.
IV Cep VB B (A 16m; B 2.1", 191deg).
IW Cep Min II 13.7; Min II - Min I = 0.52P.
IX Cep d = 0.03P. Min II 17.0.
KL Cep d = 0.019P.
KP Cep Depth of Min II 0.03m.
KV Cep Min II 14.3.
KY Cep Flare with 65
sec duration.
THere is a blue object on the place of
the flare [0001].
KZ Cep VB (8.6m, 8.6m; 1.9", 348deg).
Depths of spectral lines vary
P = 0.212938d [6488].
LL Cep Min II 14.0.
LM Cep Min II 12.8.
LP Cep Min II 13.8; Min II - Min I = 0.55P.
LO Cep Eastern
component of a double star.
LU Cep VB.
LW Cep Depth of Min II 0.05m.
LZ Cep Min II 5.63. In the Table - P(Vr)
[4627].
MN Cep Depth of Min II 0.08m?
MQ Cep Min II 15.7.
MT Cep Min II 15.5.
MX Cep SB (P = 16.03d) [8947].
MY Cep In the cluster NGC 7419.
Emission OH, H2O.
MZ Cep In the region of the cluster
NGC 7419.
NN Cep Min II 8.52.
NR Cep Min II 13.6; d = 0.025P?
NS Cep Depth of Min II 0.04m.
NW Cep Preceeding
component of a close VB. Min II 10.7.
NY Cep VB A (B 10.33m, 10", 190deg); d = 0.003P; SB2, e =
= 0.49; delta(gamma) = gamma2 - gamma1 = 32 km/s [7412].
OS Cep Very red.
OT Cep Min II 13.3.
OZ Cep Red.
PS Cep In the region of the cluster
NGC 7380. SB 2 (P = 2.09168d) [5479].
PV Cep See EH Cep. At the apex of the
bright variable fan nebula.
PW Cep See FU Cep.
QZ Cep The map of surroundings
given in [4015] for BV 323 is in reality the map
for BV 324 = QZ Cep. Min II 11.9.
V 338 Cep Min II 9.52.
V 342 Cep B - V = +3.6.
V 344 Cep B - V = +4.4.
V 345 Cep B - V = +5.0.
V 346 Cep B - V = +4.6.
V 347 Cep B - V = +4.5.
V 351 Cep VB A (B 13m, 20", 135deg). P var. Max = 2430615.57 +
+ 2.80511d*E (JD2429160 - 34300); Max =
= 2435749.12 + 2.80556d*E (JD2435310 - 40885)
[2830]. Since JD2442020 -
See Table.
bet Cep VB A (A 6m, 0.204", 47.2deg, 1977. 9; B 7.84m, A2V,
13.6", 250deg). SB 1 (Porb = 10.893d) [6486]. P var.
Max(Vr) = 2417359.715 + 0.1904795d*E (JD
2415750 - 22000); Max(Vr) = 2422203.790 +
+ 0.1904844d*E + 2.9440d*10**-11*E**2 + 3.2671d*10**-17*E**3
(JD2422000 - 42630) [0177].
Elements given in the Table satisfy obser-
vations in 1967 - 69.
del Cep VB A (B 13.0m, 20.0", 285deg; C 6.10m - 6.37m, B7IV,
41.0", 191deg. P var. Max = 2393659.856 + 5.366438d*E
(JD2372200 - 96900); Max = 2413960.73 +
+ 5.366386d*E (JD2396900 - 2414050); sin-
ce JD2414050 - see Table.
All observations in the interval JD
2373090 - 45000 are well represented also by the
elements with a square term: Max = 2442756.490 +
+ 5.366270d*E - 7d*6*10**-9*E**2 [8632].
eps Cep VB A (B 9.5m, 127.8", 15deg, 1918).
Multiperiodicity: P2 = 0.068073d
(A2/2 = 0.0061m), P3 = 0.011823d? (A3/2 = 0.0022m);
A1/2 = 0.0079m.
mu Cep VB A (B 12.3m, 19.4", 262deg; C 12.7m, 41", 299deg).
THere is also the cycle with 4400d
duration [8957].
W Cet S 5.5/2 e.
RR Cet [Fe/H] = - 1.26. P var. During JD
2417500 - 28820 Max = 2417501.444 + 0.55302577d*E;
since JD2433180 - See Table.
According to
[8726], the graph of O - C deviations from the ele-
ments given in [3506] is approximately sinusoidal,
with Pi = 2600d and the amplitude 0.025d.
RU Cet (k - b)2 = 0.01. delta(m) var? P var [2455]. Max =
= 2426964.019 + 0.5863003d*E (JD2426500 - 28430)
[0181]; Max = 2434143.056 + 0.5862676d*E (JD
2433100 - 35820) [2431]; since JD
2435820 - see Table.
RV Cet delta(S) = 9.
RW Cet Min II 10.5. P var. During JD
2426500 - 41000 Max = 2426585.503 + 0.9751814d*E
[0001]; since JD2441000 - see
Table.
RX Cet delta(S) = 5. P var. Before JD2428500 Max =
= 2425938.271 + 0.5737100d*E [3506]; since
JD2430000 - see Table.
RZ Cet delta(S) = 6.7. P var. During JD
2426585 - 28630 Max = 2426585.448 + 0.510633d*E
[3506]; current elements -
see Table.
SS Cet d = 0.025P. P var. Min = 2429321.250 + 2.9739509d*E
(JD2427340 - 30700) [2419]; Min = 2430698.160 +
+ 2.973992d*E (JD2429300 - 36650) [3115];
since JD2440000 - see Table.
SV Cet Min II 14.9.
TT Cet Min II 11.1.
TU Cet D = 0.043P. Min II 10.9. Min II - Min I = 0.478P.
According to [3564], the spec-
trum is K2.
TV Cet Min II 9.10. DII = 0.03P. Min II - Min I = 0.494P.
TW Cet Min II 11.14. P var. Min I = 2430965.595 +
+ 0.316852d*E (JD2427650 - 31000) [0192]; Min I =
= 2433611.3121 + 0.316846d*E (JD2433530 - 615)
[0001]; since JD2440000 -
see Table.
TX Cet B - V: +0.34, +0.37. Min II 11.12.
TY Cet Min II 12.1.
UU Cet (k - b)2 = 0.08. P var. Blazhko effect?
UV Cet VB B (A 12.45m, dM5.5 e; a = 2.1", P = 25a).
VV Cet Min II 11.0. EB type
is also possible.
RR type with twice shorter
period is not excluded.
VX Cet d = 0.026P.
VY Cet Min II 11.70.
VZ Cet ADS 1778 B (B 0.61", 122deg; A = omikron Cet).
Small variations
are also observed on the time scale of several
hours, with superimposed 10 - 15 minute variations
and rare flares of approximately 2 minute durati-
on [6492]. A possible white dwarf with an accre-
tion disc [8926].
WW Cet VR var (P = 0.160d) [4712].
Rapid oscillations ( ~ 10 min) of brightness are observed
[4709].
WZ Cet Min II 11.0.
XY Cet d = 0.02P. Min II 9.34.
YY Cet Min II 9.2.
ZZ Cet 4 stable oscillations are observed simulta-
neously: P1 = 213.132605s, P2 = 212.768427s, P3 =
= 274.250814s, P4 = 274.774562s.
AA Cet ADS 1581 A (B 7.7m vis, SB 2, F5, 8.5", 304deg).
Min II 6.7:. dII = 0.065P.
AB Cet ADS 1849 A (B 9.30m, 12", 293deg). SB? (VR var,
P = 2.997814d).
The period of magnetic variations is 15.9d
[8932].
AD Cet ADS 180 A (B 10m, 3", 4deg).
del Cet Nonlinear term:
+ 2.20d*10**-11*E**2.
omi Cet ADS 1778 A (B = VZ Cet, 0.61", 122deg). Maser
SiO, OH, H2O.
S Cha VB A (B 9.29m, 23", 134deg).
T Cha Occasionally quasipe-
riodic light changes are observed with periods
3.2323d, 3.4375d, 4.1800d, 3.2436d operating du-
ring 6 - 26 cycles. IR excess.
Z Cha VB A (B 5.6"). Eclipses: Min =
= 2440264.68232 + 0.0744992195d*E + 7.88d*10**-13*E**2
[8938]. D = 0.065P; d = 0.026P. Depth
of Min: 1.73m - 2.11m B before the
eclipse; 1.38m - 1.97m B after
the eclipse.
Periodic variations
during Min light [7000]. Variations with P = 27.7s
during a supermaximum [8049].
RS Cha EA/DM. Min II 6.53.
One of the compo -
nents is a pulsating variable of DSCT type. P is
in the range from 0.074d to 0.097d [8403]. delta(M) =
= 0.01m + 0.03m in the combined light.
RW Cha Min II 14.6.
RY Cha Min II 14.0.
RZ Cha Min II 8.8. DII = 0.11P.
SY Cha Quasiperiodic variations were observed. (P =
= 6.2d [4305], P = 7.6d [8946]).
TW Cha Quasiperiodic variations (P = 8.68d [4462]).
VW Cha IR excess.
VZ Cha Quasiperiodic
variations (P = 7.27d).
YZ Cha delta(m) (Min II) = 0.4m.
CG Cha Min II 14.4.
CH Cha Min II 15.1.
CX Cha Min II 15.5. Uncertain elements.
CY Cha Min II 14.0.
CZ Cha Min II 14.6.
DD Cha Min II 14.7.
DG Cha Min II 14.5.
zet Cha SB.
S Cir Min II 10.9.
T Cir Min II 9.4.
U Cir P var. Before JD2417000 Max = 2412560 +
+ 151d*E.
V Cir Min II 11.0. According to [0210],
varies in the range
10.8m - 13.0m pg.
TW Cir Min II 13.3.
UY Cir Red.
UZ Cir Epoch of main Max is given. Resembles R Cen.
Max I - Max II = 160d.
VX Cir P var. Before JD2418000 Max = 2414360 +
+ 427d*E.
AQ Cir Possibly EW type with twice longer
period.
AR Cir The magnitude in
Min light possibly corresponds to an unresolved
companion.
AT Cir d = 0.02d:.
AX Cir SB. VB? (6.5m; 6.5m; 0.5", 143deg, 1913).
BD Cir Min II 9.5.
BF Cir Min II 8.9.
BG Cir Min II 10.3.
BN Cir Deep Min II.
Twice shorter period is not excluded.
BR Cir Cir X - 1.
Cir X - 1. According to [8951],
The object does not coincide with the star (B =
= 22.5m) labelled as l in the chart in [2911] but is
situated in ~ 1" to the south of it and has m > 23.5m
on IIIA-J plates. Gradual increase of X-ray inten-
sity is periodically stopped by an abrupt intensity
fall. The moments of such transitions T are repre-
sented by the elements T = 2443292.118 + 16.595d*E
[2926]. The X-ray intensity falls are accompani-
ed by IR and radio bursts. Vr (e alfa) = +250 km/s. In
25' from the supernova remnant G 321.9 - 0.3.
tet Cir VB (6.2m, 6.2m, 0.1", 96deg).
T Col SiO maser.
U Col Min II 10.5.
Y Col V2 (NGC 1851).
Z Col V1 (NGC 1851).
RS Col Min II 9.97. dII = 0.021P.
RY Col (k - b)2 = 0.10. P var; nonlinear
term: -3.38*10**-9*E**2.
RZ Col Min II 11.20.
TV Col 2A 0526 - 328. VB A (B 15.79m, 10", 330deg).
Epoch of Max
of short-term photometric variations is given. The
following elements describe, respectively, moments
of Max Vr for balmer lines and moments of Max
for the comparatively long-term photometric varia-
tions which are due to the beat phenomenon for
the photometric and spectral periods: Max Vr =
= 2444227.631 + 0.228600d*E; Max = 2444191.5 +
+ 4.024d*E.
Flickering up to 0.15m B and flares up to
0.3m U are also observed [8960].
R Com Emission.
S Com delta(S) = 8.
T Com OH, H2O emission.
U Com delta(S) = 5.
V Com P var. Max = 2424518.219 + 0.46913844d*E (JD
2420900 - 26900) [0218]; since JD
2438100 - see Table. delta(S) = 8.
W Com Radio source ON 231.
X Com Z = 0.092. Spectrum description [7415, 8966].
Y Com In the region of
the globular cluster M 53 (NGC 5024).
Z Com See Y Com.
RR Com See Y Com.
RS Com In the region of
the globular cluster NGC 5053.
RT Com See RS Com. A var; P var. Max =
= 2423113.496 + 0.5651925d*E (JD2422700 -
- 26450) [0222]; since JD2438535 -
see Table.
RU Com See Y Com.
RV Com See Y Com.
RW Com See CT Com. dI = 0.04P; Min II 11.56. P var.
Min I = 2433040.406 + 0.23734705d*E (JD
2419680 - 34550) [0185]; since JD
2439600 - see Table.
RY Com P var. Max = 2425007.450 + 0.46894835d*E (JD
2425000 - 27500) [3506]; Max = 2432674.390 +
+ 0.4689397d*E (JD2432600 - 38110) [3415];
since JD2438100 - see Table.
(k - b)2 = 0.07.
RZ Com Possible member of the Comae Berenices clus -
ter. Min II 11.09; dI = 0.043P, dII = 0.039P. P var.
Min I = 2433396.737 + 0.33850556d*E (JD2425000 -
- 33300) [0226]; since JD2433300 -
see Table.
Shape of the light curve varies.
SS Com Min II 11.9.
ST Com delta(S) = 10.
SX Com In the region of
the globular cluster NGC 4147.
SZ Com See SX Com.
TU Com Shape of
the light curve, A and P vary. Mean elements
are given in the Table. Possible period of Bla-
zhko effect is 75d [3584]. [Fe/H] = -1.43.
UU Com Member of the Comae Berenices cluster.
Light variations are due to rotation and pulsati-
ons of the star. Rotational period is 2.1953d or
1.0256d or 0.9178d. Period of pulsations is 0.0227d
(A ~ 0.01m). According to [7985] there are two pe-
riods of pulsations: P1 = 0.0274d and P2 = 0.0209d
(P2/P1 = 0.76).
UV Com [Fe/H] = -1.44.
UW Com [Fe/H] = -1.22.
UX Com Min II 10.13. P var; nonline-
ar term: - 3.75d*10**-8*E**2.
UY Com [Fe/H] = -1.51.
UZ Com [Fe/H] = -1.44.
VV Com [Fe/H] = -1.53.
VW Com VB (12.00m, dM 3.5e; 12.3m, dM 4e, 3.0", 23deg, 1945).
Range of total brightness variation
is given. According to [8363] the component B is
variable. However both components may be vari -
ables.
VY Com Min II 14.5.
AI Com Member of
the comae berenices cluster. VB A (B 6.63m,
145", 251deg). Pulsations
are possible: P = 0.052d (A = 0.02m) [8975].
AL Com Within 8' to the south-east from
the nucleus of M 88 (NGC 4501) galaxy.
AQ Com Min II 15.7.
BM Com Min II 13.8.
BS Com P var. Max = 2434453.31 + 0.36341d*E (JD
2434130 - 35230); since JD2435590 -
- see Table.
Shape of the light curve varies.
BZ Com [Fe/H] = -1.21.
CC Com See CT Com. Min II 12.09; dI = 0.03P.
CD Com [Fe/H] = -1.78.
CF Com Shape of the
light curve varies.
CG Com [Fe/H] = -1.06.
CI Com RRC?
CK Com P var. Max = 2437370.71 + 0.6940159d*E (JD
2437370 - 40130); Max = 2441630.35 + 0.6939080d*E
(JD2440130 - 41630); since JD
2441630 - see Table.
Blazhko effect. [Fe/H] = -1.68.
CL Com [Fe/H] = -1.00.
CN Com Min II 13.5.
CP Com [Fe/H] = -1.19.
CT Com In the region of the Comae Berenices cluster.
CV Com See CT Com.
CX Com See CT Com. Not member of the cluster.
DD Com Min II 14.90.
DG Com Min II 14.6.
DL Com P var?
DR Com EW? P = 0.45184d?
DS Com [Fe/H] = -1.32.
DT Com [Fe/H] = -1.60.
DU Com [Fe/H] = -1.45.
DV Com [Fe/H] = -1.57.
DW Com [Fe/H] = -1.53.
EE Com P = 0.539533d
Also satisfies observations. [Fe/H] = -1.64.
EF Com [Fe/H] = -1.90.
EG Com [Fe/H] = -1.29.
EI Com [Fe/H] = -1.68.
EL Com P = 0.52362d
Also satisfies observations.
EM Com [Fe/H] = -1.64.
EN Com [Fe/H] = -1.19.
EO Com [Fe/H] = -1.51.
EP Com [Fe/H] = -0.98.
EQ Com Min II 15.3.
ER Com [Fe/H] = -1.51.
ES Com [Fe/H] = -2.02.
EW Com [Fe/H] = -1.77.
EX Com P = 0.558359d? [Fe/H] = -1.48.
EY Com Min II 18.0.
EZ Com P = 0.568349d? [Fe/H] = -1.16.
FG Com P = 0.3098d
Also satisfies observations.
FK Com Wide emission lines H alfa and H, K CaII
of variable intensity. Epoch of light minimum is
given.
FM Com The member
of the Comae Berenices cluster.
Multiperiodicity.
Cycle of 0.0713d was observed
also [8989].
FO Com See CT Com.
FP Com See CT Com. mu = 0.23", P = 158deg. Red.
FZ Com P = 4.704864d?
GM Com See CT Com.
GN Com Member of
the Comae Berenices cluster. P > 1d.
GO Com See CT Com.
GP Com mu = 0.38", p = 286deg. SB (Porb = 0.032306d).
Unique object G 61 - 29. Consists of two interac-
ting white dwarfs. The lower mass star, a helium
white dwarf, transfers mass to the higher mass
star surrounded by an accretion disk. Usually fla-
res are being observed with an amplitude about
0.2m V, 0.5m U lasting about 20 seconds [7417,
8991]. Sometimes periods of photometric activi-
ty arise when amplitude of light variations rea-
ches 0.6m V and sharp passages from maxima to
minima are being observed; the duration of these
minima reaches up to 0.14d [7417]. When the star
is most active, periodic light oscillations appe -
ar with P = 105 seconds And amplitude 0.05m -
- 0.10m V [7062].
GQ Com Z = 0.165. Emission H, [OIII].
Irregular light variations.
= + 0.16.
HH Com Epoch of Min in V system is given.
HI - HK Com
See CT Com.
HM - HW Com
See CT Com.
R CrA In the head of the
bright cometary nebula NGC 6729. IR excess.
S CrA VB A (B 13.5m, 1", 137deg). IR excess.
T CrA In the bright cometary nebula
NGC 6729. IR excess.
V CrA Quasiperiodic variations (P ~ 75d, delta(V) ~ 0.2m - 0.9m). IR
excess.
RS CrA sp of two close stars; each of
them or both may be identified with CoD -39deg 13082.
RW CrA Min II 9.4.
SS CrA V1 (NGC 6541).
SV CrA The period may be twice shorter.
TY CrA VB A (B 13.3m, 4", 138deg; C 58", 24deg).
In the bright nebula NGC
6726/27. P = 1.92D is not excluded, in that case
Min II = Min I. On the basis of visual observations
8.7 - 12.4 v (presumably "spurious variability"
due to the difficulties of estimates over the
bright background of the nebula), and the star
was classified as INSA.
TZ CrA Min II 9.72.
UU CrA Min II 11.0.
UX CrA See SV CrA.
UY CrA P var?
VV CrA In the region of the bright nebula NGC
6729. IR excess.
AF CrA P var. Before JD2418060 Max = 2413710 +
+ 483d.*E; since JD2418060 -
see Table.
AL CrA B - V: +0.65, +1.30. [A/H] = -0.2.
AN CrA P var. Nonlinear term:
- 0.006d*10**-6*E**2.
AU CrA P var. Nonlinear term:
-0.026d*10**-6*E**2.
AY CrA Min II 15.2.
BG CrA Min II 15.1.
BH CrA P var. Nonlinear term:
-0.023d*10**-6*E**2.
CM CrA P var. Nonlinear term:
-0.007d*10**-6*E**2.
CR CrA Min II 15.7.
CS CrA Min II 15.2.
CY CrA P var. Nonlinear term:
-0.002d*10**-6*E**2.
DG CrA See VV CrA.
DL CrA Min II 13.6.
DN CrA P var. Nonlinear term:
+0.006d*10**-6*E**2.
DZ CrA d = 0.02P.
EE CrA var, 13.5m - 15.5m, P2 = 3000d - 5000d
delta(m) (P1 = 167d) ~ 1.5m.
EK CrA P var. Before JD2422600 Max = 2411870 +
+ 421d*E.
FF CrA Before JD2423000 Max = 2411530 + 140.2d*E.
FK CrA Min II 14.5.
FS CrA Min II 14.5.
FW CrA Before JD2416600 Max = 2411190 + 112.2d*E.
GS CrA Before JD2422600 Max = 2414070 + 284d*E.
IT CrA Min II 13.6.
KQ CrA [A/H] = -0.7. B - V: +0.76, +1.23.
KT CrA Red.
Lu CrA P = 182d is possible.
MS CrA Yellow.
MT CrA Min II 13.1.
NO CrA Reddish.
QR CrA eddish.
V 347 CrA B - V: +0.82, +1.17.
V 350 CrA Min II 13.4.
V 385 CrA The period
may be spurious.
V 413 CrA (k - b)2 = 0.11.
V 428 CrA See SV CrA.
V 449 CrA [A/H] = -0.3.
V 454 CrA Min II 10.5.
V 455 CrA d = 0.05P. Min II 13.7.
V 457 CrA Epoch of Min is
given. EW type is also possible, in that case
the value of P should be doubled.
V 465 CrA Min II 14.2.
V 467 CrA P var?
V 471 CrA Min II 13.3.
V 478 CrA Sometimes a cycle 60d - 70d.
V 480 CrA Min II 13.9.
V 490 CrA P var?
The elements represent the observati-
ons of 1944.
V 493 CrA P var?
V 501 CrA Min II 13.4.
Twice shorter period is possible.
V 503 CrA d = 0.03P.
V 511 CrA Twice lon-
ger period is possible.
V 512 CrA P var?
V 513 CrA Min II 13.2.
V 514 CrA Min II 14.0.
V 527 CrA P var.
V 535 CrA P var.
V 541 CrA P var?
V 545 CrA VB.
Combined brightness with a faint com-
panion is given.
V 553 CrA P var?
V 566 CrA Min II 12.7.
V 568 CrA Sometimes a cycle 60d - 80d.
V 569 CrA Min II 13.1. EB type is
possible.
V 571 CrA Min II 14.7.
V 572 CrA Min II 14.0.
V 577 CrA Min II 13.2.
RR type with twice shorter period
is possible.
V 578 CrA RV type with
P = 118d is possible.
V 580 CrA Min II 14.4.
V 595 CrA P var.
V 601 CrA Epoch of min is given.
V 603 CrA Slightly
noticeable Min II at the phase 0.5P.
V 604 CrA d = 0.03P.
V 607 CrA Min II 14.3.
V 612 CrA d = 0.03P.
V 615 CrA P var?
V 622 CrA Sometimes 55d - 60d
cycles.
V 633 CrA P var.
V 634 CrA Min II 13.9.
V 648 CrA Min II is
felt at the phase 0.5P.
V 659 CrA P = 189.4d is possible.
V 667 CrA In the region of the bright cometary ne-
bula NGC 6729. The spectral type is earlier
than K.
V 676 CrA RR type is possible.
V 686 CrA Max I 5.34, Min I 5.41, Max II 5.35, Min II 5.40
[8970].
V 691 CrA 4U 1822 - 37. Emissions
CIII/NIII lambda 4640 - 50, He II lambda 4686, CIV lambda
1550 etc.
V 692 CrA P = 0.83d is possible.
eps CrA Min II 4.95.
R CrB IR excess.
S CrB OH, H2O, SiO maser.
T CrB VB? A (B <= 12m, 0.2"). SB (P = 227.6d).
The spectral period is present in the photomet-
ric data of 1891 - 1917 and 1960 - 1971 [8978]. The
epoch of the first outburst JD2402734 (1866).
Two smaller outbursts were observed in UV light,
JD2438030 (1963) and 2442543 (1975) [8979].
U CrB Min II 7.72. P var.
RR CrB P2 = 377d. delta(m) (P1) ~ 0.5m, delta(m) (P2) ~ 0.6m.
RS CrB P2 = 69.5d [1100].
Main period oscillation: 9.1m - 11.6m.
RT CrB Nonlinear term:
+ 2.01d*10**-8*E**2. Min II 10.52 (var). DII = 0.09P.
RV CrB P var. Max = 2428285.608 + 0.3316217d*E (JD
2428285 - 31610); Max = 2431705.349 + 0.3317313d*E
(JD2431705 - 32954); Max = 2433030.572 +
+ 0.331705d*E (JD2433030 - 36814) [5496]; Max =
= 2440001.453 + 0.331569d*E (1967 - 1971) [6237];
Max = 2441451.413 + 0.331619d*E (1972 - 1974)
[7032]. The Table gives current elements. On
the period changes see also [3506]. Blazhko effect?
RW CrB d = 0.028P. Min II 10.29.
TW CrB Min II 11.0.
TZ CrB ADS 9979 A (B 6.72m, GIV, 6.6", 233deg, 1980).
SB 2 (P = 1.139789d).
Epoch of
Min is given. The variation presented in the Tab-
le is superimposed by a second one, with the sa-
me amplitude and P = 0.1d. The amplitude is given
for the combined light of ADS 9979 A and B, the
mean magnitude is for ADS 9979 A.
UU CrB During JD2444381.73 - 76 a slow flare was ob-
served, with maximal amplitude 0.30m in the IK
band and 0.18m in the U band.
alf CrB lambda eff = 7230 A: DI = 0.034P, DII = 0.018P, Min II - Min I =
= 0.66P, depth of Min I 0.10m, Min II 0.025m.
bet CrB VB A (B ~ 5m - 6m, 0.2", ~ 130deg, 1978). SB
(P = 3833.7d). Magnetic field
var, P = 18.487d. The
epoch of Min light is given.
gam CrB ADS 9757 (4.2m, 5.6m; A = 0.74", P = 91.0a).
U Crv VB A (B 13.5m, 0.4' p).
W Crv Min II 11.86.
The light curve
is asymmetrical, the maxima differ in hight by
0.10m.
Y Crv Min II 11.7.
RRC type with twice shorter period
is possible.
Z Crv d = 0.06P.
RV Crv Elements do
not satisfy some of the published moments of Min.
RZ Crv Min II 13.9.
SX Crv Min II 9.23.
The
shape of the light curve varies. Depth of Min I
0.20m, depth of Min II 0.18m. In 1972 the system
became fainter than in 1971 by 0.06m.
R Crt Periods of light constancy which last up to 250d oc-
cur every two or there thousand days. OH, H2O
maser.
S Crt H2O maser.
T Crt Mean light var, P2 = 1006d.
V Crt Min II 10.1; Min II - Min I = 0.57P.
W Crt (k - b)2 = +0.21.
X Crt (k - b)2 = +0.02.
Z Crt d = 0.016P.
RR Crt P = 293d or 146d is possible. .
RV Crt Min II 9.4:.
SU Crt [Fe/H] > -0.3.
SV Crt ADS 8115 A (B 11.5m vis, 1", 220deg). SB 2 (P =
= 5.90513d, apsidal motion,
P ~ 700a).
Epoch of
Min I in B light is given. Depth of Min II is 0.015m.
EuII and SrII in emission.
R Cru In the region
of the open cluster NGC 4349.
T Cru See R Cru.
U Cru P var. Max = 2410143 + 351.4d*E (JD2410100 -
- 14100) [0237]; since JD2437600 -
see Table.
W Cru Min II 9.3.
SU Cru [A/H] = -0.8.
SV Cru In the region
of the open cluster Ruprecht 97.
Non-member of the cluster.
SW Cru VB A (B 14.0m, 12"). (k - b)2 = 0.27.
SY Cru d = 0.05P?
TU Cru Min II 11.5.
TW Cru Min II 12.85:.
TX Cru It is not ex-
cluded that actually P is much shorter, close to
1d, for instance.
TZ Cru P = 2.091140d?
UW Cru Min II 12.9; Min II - Min I = 0.536P.
UX Cru VB A (B 10"). Min II 12.4; Min I - Min II = 0.325P;
DII = 0.025P.
VY Cru Min II 13.5.
VZ Cru P = 1.125810d?
WW Cru Min II 13.0.
WX Cru d = 0.040P.
Light variability in maximum is no-
ted.
WY Cru VB A. P = 9.013290d?
XX Cru P = 3.28566d?
XY Cru Min II 11.7.
XZ Cru P = 1.6495930d?
YY Cru Min II 13.0.
YZ Cru Min II 13.1.
ZZ Cru Min II 9.8.
AB Cru Min II 8.9.
AC Cru Min II 12.1.
AD Cru VB A (B 14.5m, 10", 270deg). P var. Max = 2434918.160 +
+ 6.39844d*E (JD2423800 - 35400) [2309];
since JD2441000 - see Table.
AE Cru Depth of Min II 0.03m.
AF Cru According to [1122] Algol-type with the elements:
Min I = 2424988.959 + 1.895669d*E, D = 0.06P.
This conclusion
must be checked. The star deserves careful inve-
stigation.
AG Cru The blue component is possible [9004].
AI Cru In the region
of the open cluster NGC 4103. Min II 9.94.
AG Cru Min II 13.8.
AT Cru Min II 12.6.
AW Cru Min II 13.9.
AY Cru Min II 11.2.
BB Cru Min II 14.0.
BC Cru Depth of Min II 0.03m.
BD Cru Depth of Min II 0.05m.
BF Cru Min II 12.3.
BH Cru Epoch of Min I is given in the Table. The light
curve like the light curves of R Cen and R Nor
has two maxima and two minima of different
depths. Max I 7.6m (0.22P), Min II 8.0m (0.41P),
Max II 7.2m (0.53P).
BI Cru Spectrum description [4949].
BK Cru In coalsack region.
BM Cru See BK Cru.
BP Cru 3U 1223 - 62. A unique X-system.
Consists of an X-pulsar with pulse period 698s
[9018] moving on an excentric orbit (E = 0.47)
around the ellipsoidal B2 supergiant with orbital
period of 41.51d. Accretion of the stellar wind
from the primary star on the pulsar increases du-
ring the periastron passage. Therefore large X-
flares are observed with the elements: T (X Max) =
= 2433158.09 + 41.51d*E. Optical flares are possi -
ble.
BQ Cru B - V: +1.13, +0.88.
BS - BW Cru
In the open
cluster NGC 4755.
bet Cru VB A (B 11.4m, 44.3", 322deg; C 7.5m, 372", 23deg).
Interferometric
binary.
Multiple periods (the total V amplitu-
des of corresponding oscillations are indicated
in brackets): P0 = 0.2365072d (0.034m), P1 = 0.160466d
(0.029m), P2 = 0.121383d (0.01m), P02 = 0.249373d
(0.016m), P13 = 0.24273d (0.024m), P24 = 0.23931d
(0.028m), P03 = 0.16342d (0.016m), P14 = 0.16171d
(0.029m).
tet 2 Cru SB (P = 3.4380d). BCEPS, P > 1h? [8420].
lam Cru Type ELL with
P = 0.7902d is possible. Amplitude and shape of
the light curve vary. The secondary oscillation
(A = 0.007m) with the elements Max = 2441779.034 +
+ 0.1793d*E is possible.
R Cyg VB A (B 9.3m, 91", 14deg). S 4/6e - S 8/6e.
T Cyg VB A (B 10.03m, 10.2", 122deg; C 12m, 13.6", 197deg).
U Cyg VB A (B 7.8m, 63.5", 51deg). P var. Max = 2406455 +
+ 461.57d*E (JD2404590 - 13900); Max = 2414827 +
+ 470.76d*E (JD2413900 - 19940); Max = 2421806 +
+ 455.95d*E (JD2419940 - 27380); Max = 2427848 +
+ 472.85d*E (JD2427380 - 35750); since JD
2435750 - see Table.
W Cyg There is
a second oscillation with P = 235.3d.
X Cyg P var. Max = 2410190.86 + 16.3841d*E (JD2410100 -
23370) [9028]; since JD2417000 -
see Table.
There is a square term in the elements gi-
ven in the Table: + 1.01d*10**-7*E**2.
[A/H] = 0.4.
Y Cyg Min II 7.75; E = 0.1458. Apsi-
dal motion: P = 47.6 yr.
There
are sinusoidal terms in the elements: +0.1391d sin
(0.06256deg*E) -0.0076d sin 2 (0.06256deg*E); Min II =
= 2409454.9174 + 2.9963328d*E - 0.1391d sin (0.06256deg*E) -
- 0.0076d sin 2 (0.06256deg*E).
Z Cyg OH, H2O emission.
RR Cyg VB A (B 12.5m, 18.1", 58deg).
RS Cyg VB A (B 7.09m, 132", 355deg; C 9.3m, 56", 106deg).
Epoch of light minimum is
given. The shape of the light curve strongly varies.
Double maxima are sometimes observed (Min II at the
phase 0.5P).
RU Cyg VB A (B 12.40m V, 10", 224deg; C 11.15m V, 19", 29deg).
RV Cyg VB A (B 10m, 142", 118deg).
RY Cyg In the region of the
open cluster NGC 6883.
RZ Cyg The shape of the light curve strongly varies. Alternation
of high and low maxima, as well as of shallow and
deep minima is observed, as a rule: 9.8m <= Max <= 12.0m.
11.8m <= Min <= 14.1m.
SS Cyg SB 2 (P = 0.27512995d [8285]).
During maxima of brightness there are oscillations of
light and X-ray flux with amplitudes about 0.002m V
and periods changing between 7.29s and 10.90s [6102,
9032].
SU Cyg P var. Max = 2421278.503 + 3.845507d*E (JD2414250 -
29000) [1559]; Max = 2433095.944 + 3.845664d*E (JD
2429000 - 33150) [0921]; since JD2434500 -
see Table.
SV Cyg VB A (B 9.5m V, 145", 140deg).
SW Cyg Min II 9.30; d(V) = 0.018P; d(U) = 0.00P. P var. Min I =
= 2414782.448 + 4.572937d*E (JD2411340 - 16450);
Min I = 2418440.758 + 4.5727923d*E (JD2417060 -
19740) [0063]; Min I = 2421504.489 + 4.572729d*E (JD
2421470 - 24970); Min I = 2425185.550 + 4.5728386d*E
(JD2424960 - 29500); Min I = 2433160.669 + 4.5729841d*E
(JD2433000 - 36800) [9085]; Min I = 2438584.3081 +
+ 4.57311736d*E (JD2438600 - 40560) [9085];
since JD2441160 - see Table.
SY Cyg d = 0.040P. Possible depth
of Min II 0.03m.
P var. Min I = 2411659.568 + 6.00584d*E (JD2411600 -
17100); Min I = 2420001.571 + 6.005716d*E (JD
2418760 - 20760) [1961]; Min I = 2437069.254 + 6.005626d*E
(JD2432800 - 37070) [5416].
Mean elements given in the Table represent epochs of
Min I in the interval JD2414400 - 37070 up to +- 0.07d.
According to [4248] the apsidal motion with the pe-
riod ~ 46 years is possible.
SZ Cyg [A/H] = 0.5. P var [2392].
Mean elements given in the
Table represent epochs of Max up to +- 0.5d. According
to [9029] "the O - C diagram has a sinusoidal struc-
ture as is to be expected for a member of a binary sy-
stem" with P orb = 65 years.
TT Cyg VB A (B 10.8m V, 70", 213deg; C 11.1m V, 83", 49deg;
D 10.7m V, 94", 268deg).
TV Cyg According to [3663] - spectrum G0.
TX Cyg [A/H] = -0.2. P var. Max = 2436793.138 + 14.708157d*E
(JD2415000 - 37000); since JD2436700 -
see Table.
UU Cyg VB A (B 10.7m V, 3.6", 351deg).
UV Cyg VB A (B 10.8m V, 0.9", 79deg).
UW Cyg P var. Min I = 2419624.501 + 3.450797d*E (JD2410000 -
20750) [0526]; Min I = 2419624.501 + 3.450752d*E (JD
2419620 - 33000); Min I = 2433848.508 + 3.450740d*E
(JD2430000 - 41800); since JD2441800 -
see Table. Possible depth of Min II 0.05m.
UX Cyg P var. Max = 2432444 + 560.3d*E (JD2415670 - 32450);
Max = 2439352 + 578.0d*E (JD2432450 - 40500);
since JD2437600 - see Table.
Sometimes rapid light dec-
reases on the ascending branch near Max are observed
[1563, 1564]. H2O, OH, SiO maser.
UY Cyg delta(S) = 3.8.
UZ Cyg VB A (B 10.8m, 28", 130deg). d = 0.032P; Min II 10.31.
VV Cyg Min II 13.2. P var? [3665].
VW Cyg d = 0.035P; Min II 10.31. P var. Min I = 2417377.123 +
+ 8.4305260d*E (JD2415660 - 17400); Min I =
= 2430444.061 + 8.4302826d*E (JD2417400 - 30450);
Min I = 2441116.868 + 8.4303917d*E + 4.31d*10**-8*E**2 (JD
2430450 - 41120) [7096]; since JD2440350 -
see Table.
VX Cyg [A/H] = 0.2. P var. THere is a square term in the elemenmts
+ 8.02d*10**-7*E**2.
VZ Cyg P var. Max = 2437103.945 + 4.8645598d*E(JD 2416000-
41000); since JD 2434000 - see Table.
WW Cyg d = 0.008P; Min II 10.16. P var [6144]. Mean elements:
Min I = 2416981.299 + 3.3176924d*E (JD 2412000 -31000)
[0063]; since JD 2431000 - see Table.
WZ Cyg Min II 10.9.
XX Cyg [Fe/H] = -0.49. P var. Max = 2430671.1010 +
+ 0.134865026*E(2416560 - 30000); since J D 2430000 - see Table.
XZ Cyg [Fe/H] = -1.2. P var. Max = 2417201.241 + 0.4665878*E -
- 0.000107d*10**-6*E**2 (JD2414000 - 35000) [2550];
Max = 2438562.796 + 0.466570d*E (JD2434000 - 39800);
Max = 2440445.789 + 0.466497d*E (JD2439800 - 41000)
[6237]; Max = 2441453.3856 + 0.4664731d*E (JD
2441000 - 42500) [7424]; Max = 2443028.641 +
+ 0.466438d*E (JD2442500 - 43800) [9101]; Max =
= 2444142.650 + 0.466649d*E (JD2443800 - 44200)
[9102]; since JD2444100 - see
Table.
Besides that the star has a strongly
expressed blazhko effect; the period of Blazhko ef-
fect varies, too [7424, 7425]. 0.13P <= M - m <= 0.22P; 0.90m <=
<= A(B) <= 1.70m, 0.70m <= A(B) <= 1.30m; - 0.05P < O - C < +0.05;
Max A = 2417025.5 + 57.401d*E (JD2417000 - 38500);
Max A = 2438881.7 + 58.387d*E (since JD
2438500).[9103].
After JD2444000
Blazhko effect period probably decreased to 56.3d [9102].
ZZ Cyg VB A (B 12.63m, 8.5", 43deg.
Total brightness variation range
is given. Min II 10.78. P var. Min I = 2417442.419 +
+ 0.6286185d*E (JD2415000 - 25800) [7427];
since JD2427950 - see Table.
AA Cyg S 6/3.
AC Cyg H2O maser.
AD Cyg S 5/5.
AE Cyg d = 0.039P; Depth of Min II 0.06m.
AF Cyg Light curve (1914 - 1956) [9104].
Two more independent oscillations are super-
imposed: P2 = 175.8d, P3 = 941.2d.
AK Cyg VB A (B 11.06m, A7, 20", 85deg).
AV Cyg P var. Max = 2420451.9 + 87.48d*E (JD2418782 -
24823); Max = 2427936.3 + 89.73d*E (JD2426326 -
28745); Max = 2429440.9 + 87.69d*E (JD2428820 -
31260); Max = 2436413.8 + 89.63d*E (JD2434610 -
37130); since JD2437450 - see
Table. 0.27P <= M - m <= 0.50P.
AX Cyg VB A (B 10.2m, 18", 52deg).
AY Cyg In the region of the
open sluster Dolidze 2.
BB Cyg P var. Max = 2426360 + 265.7d*E (JD2414900 - 26700);
Max = 2433091 + 258.6d*E (JD2426700 - 35500); Max =
= 2438354 + 266.9d*E (JD35500 - 40200) [9106];
since JD2439200 - see Table.
BF Cyg P orb = 750d [5655].
Irregular light variations and sometimes observed
brightenings by 2m - 3m are superimposed by semire-
gular oscillations with the cycle 755d [1039, 8044].
BG Cyg P var. Max = 2421190 + 290.35d*E (JD2421150 - 29950);
Max = 2430546 + 307.3d*E (JD2429950 - 30850); Max =
= 2432872 + 289.5d*E (JD2430850 - 34920);
since JD2435100 - see Table.
BI Cyg VB A (B 9.4m, 126", 110deg).
BO Cyg D = 0.025P; Min II 12.0.
BR Cyg D = 0.020P; Min II 9.58.
BS Cyg SC 8/8. P var. Max = 2422655 + 420d*E (JD2422600 -
24750) [1161]; Max = 2425181 + 431.4d*E (JD2424750 -
26500) [1171]; since JD2437500 -
see Table.
BY Cyg VB A (B 16m).
BZ Cyg [A/H] = 0.1. Double maximum.
CD Cyg [A/H] = 0.2. P var.
There is a square term in the elements:
+ 1.54d*10**-6*E**2.
CG Cyg VB A (B 11.8m, 1.3", 306deg; 1979.7). 10.10 <= Min II <= 10.44.
P var. Min I = 2422967.4248 + 0.63114347d*E (JD
2422900 - 38500); since JD2439000 -
see Table.
Combined light range
is given. Shape of the light curve varies [8848].
CH Cyg Semiregular light variations with the mean cycle 97d;
mean brightness varies with the cycle ~ 4700d [1169].
There are also a cycle 725d [8849], rapid oscilla-
tions (A <= 0.25m U) and flares [5350]. It is not excluded
that the system is an eclipsing one [6499].
CI Cyg d = 0.084P.
Depth of eclipses ~ 0.8m. The eclipses of B star are obser -
ved. Usually there are light fluctuations near mean
brightness ( ~ 12.1m). The outbursts last some dozens
and hundreds days. Light curves [6155, 8044, 8850,
8851]. Emissions of H, He I, He II, [O III], and N III.
CM Cyg S 4/6.5e.
CU Cyg P var. Max = 2422643 + 223.8d*E (JD2422600 - 26500);
since JD2426500 - see Table.
CV Cyg dI = 0.06P; Min II 11.33. P var. Min I = 2424458.348 +
+ 0.9834523d*E (JD2414300 - 24500); since JD
2424450 - see Table.
Shape of the light curve And Min I depth vary.
CY Cyg SC 2/7.5.
CZ Cyg P var. Max = 2424500 + 284d*E (JD2424500 - 33600)
[3122]; since JD2432700 - see
Table.
DD Cyg P var. Max = 2425465 + 148.30d*E (JD2424800 - 39000)
[1149]; since JD2439000 - see
Table.
DF Cyg P var [1177, 6107]. Mean
brightness varies: Min = 2411292 + 780.2d*E [1571].
DG Cyg SiO maser?
DH Cyg OH emission?
DK Cyg dI = dII = 0.04P; Min II 10.90. P var.
Shape of the
light curve and depth of Min II vary.
DL Cyg Min II 9.9.
DM Cyg P var. Max = 2425887.560 + 0.4198557d*E (JD2415200 -
25900) [3506]; Max = 2425887.5597 + 0.41985715d*E
(JD2425880 - 29250) [0522]; Max = 2433872.420 +
+ 0.41985842d*E (JD2429250 - 37900) [3506]; Max =
= 2438677.708 + 0.4198619d*E (JD2438600 - 41250)
[7114]; since JD2441240 - see
Table.
There is also Blazhko effect with the elements:
Max(O - C) = 2442978.97 + 26.01d*E [8853]; -0.01 d< =
<= O - C <= + 0.01d. delta(S) = 0.
DQ Cyg P = 180d?
DT Cyg P var. Max = 2424305.651 + 2.49913d*E (JD2424300 -
28500) [1183]; Max = 2432792.893 + 2.49934d*E (JD
2430000 - 36000); since JD2436000 -
see Table.
DV Cyg P var. Max = 2425476 + 146.7d*E (JD2415200 - 29200);
since JD2432800 - see Table.
DW Cyg P var. Max = 2427603 + 279.6d*E (JD2416700 - 33500);
since JD2433500 - see Table.
DX Cyg Min II 14.2; Min II - Min I = 0.515P; DI = 0.22P, DII = 0.12P.
DY Cyg SLow oscil-
lations are superimposed by rapid ones with A = 0.3m
[3662]. According to [3148] type EB? Min = 2436659.531 +
+ 0.6990d(:)*E (JD2436600 - 37000) [3148].
EE Cyg Min II 14.5.
EF Cyg 142d <= P <= 175d.
EH Cyg P var. Max = 2427608 + 276.90d*E (JD2416200 - 27610);
since JD2427800 - see Table.
EI Cyg Epoch of Max I is given; heights of Max I and Max II
differ strongly, the depths of Min I and Min II are almost
equal. Max I - Min I = 52d.
EK Cyg Observations are repre-
sented by the elements in the interval JD2425200 -
37900 only.
EM Cyg Mean cycle varies in the range
19d - 33d [4248, 9111]. Depth of eclipses 0.25m V; ele-
ments of eclipsing system light variations: Min =
= 2437882.8595 + 0.29090950d*E - 21d*10**-12*E**2 [8854].
sometimes tHere are light oscillations with periods
14.6s - 21.2s and an amplitude up to 0.4% [6102, 9112].
EN Cyg d = 0.012P. P var. Min = 2425181.311 + 2.2148998d*E
(JD2424880 - 29600) [0332]; since JD2433500 -
see Table.
ES Cyg P var. Max = 2425146 + 157d*E (JD2425000 - 29300)
[0332]; since JD2432800 - see
Table.
EV Cyg P var. Max = 2427740 + 259.1d*E (JD2425100 - 29100);
since JD2433500 - see Table.
The position of the star in the chart in
[0530] is wrong [0782].
EZ Cyg P var?
Shape of the light curve and the amplitude
strongly vary; 0.40P < = M - m < = 0.48P.
FF Cyg S 5.5/6 - E.
FG Cyg P var. Max = 2426955 + 456.0d*E (JD2416000 - 27000)
[0001]; Max = 2426955 + 458.8d*E (JD2426900 - 34300)
[3122]; since JD2439200 - see
Table.
FM Cyg P var. Max = 2425313 + 274d*E (JD2425300 - 29200)
[0332]; since JD2429200 - see
Table.
FN Cyg P var. Max = 2429137 + 314.6d*E (JD2416200 - 29200)
[0001]; since JD2432800 - see
Table.
FO Cyg A var. P var. Max = 2425193 + 156.6d*E (JD2425000 -
29200) [0332]; since JD2432500 -
see Table.
FR Cyg Min II 14.0; d = 0.03P.
FT Cyg P var. Max = 2425184 + 156.7d*E (JD2425100 - 29200)
[0332]. 83d <= P <= 187d (JD2432500 - 38000).
FY Cyg P var. Max = 2425172 + 194.d*E (JD2425100 - 29300)
[0332]. 130d <= P< = 189d (JD2432500 - 38000).
GG Cyg d = 0.079P; Min II 12.1.
GM Cyg P var. Min = 2428754.305 + 4.745772d*E (JD2413200 -
33500) [1209]; since JD2433500 -
see Table.
GN Cyg P var. Max = 2425448 + 156d*E (JD2425400 - 27400)
[1155]; since JD2427500 - see
Table.
GO Cyg Min II 8.73. P var.
Intrinsic light variability
of the components is possible [1210].
GS Cyg P = 195d?
GT Cyg Depth of Min II 0.05m? P var?
GY Cyg Secondary oscillation with P = 4000d and A(V) =
= 0.5m is possible.
GZ Cyg Red.
HL Cyg d = 0.02P.
HV Cyg VB (Northern component).
HY Cyg P var. Max = 2425334 + 344d*E (JD2425300 - 29200)
[0332]; since JD2432760 - LB?
II Cyg P var. Max = 2425150 + 82d*E (JD2425120 - 25550),
Max = 2425475 + 94d*E (JD2425550 - 29250) [0332];
since JD2432500 77d <= P <= 99d.
IK Cyg P var. Max = 2425199 + 77.3d*E (JD2425000 - 29200)
[0332]; since JD2432500 - see
Table.
IT Cyg P var. Max = 2425305 + 67.4d*E (JD2425300 - 850)
[0332]; since JD2432500 - see Table.
IU Cyg B - V: +0.90, +1.45. P var. Max = 2429157.6 + 31.22266d*E
(JD2417800 - 29250); Max = 2433601.3 + 31.1550d*E
(JD2432700 - 35400); since JD2435400 -
see Table.
IV Cyg P var. Max = 2425470.406 + 0.33432871d*E (JD2425300 -
33120) [3506]; Max = 2434122.519 + 0.33433895d*E (JD
2432700 - 40200) [4248]; since JD2440200 -
see Table.
Shape of the light
curve varies: 0.10P <= M - m <= 0.20P.
IX Cyg P var. Max = 2425173 + 172d*E (JD2425000 - 25900)
[0332]; since JD2428000 - see
Table.
KL Cyg P var. Max = 2437906 + 536.8d*E (JD2418500 - 38000)
[0001]; since JD2438000 - see
Table.
KP Cyg delta(S) = 0.
KR Cyg Min II 9.37.
KU Cyg Min II 11.15; d = 0.047P.
Shape of the light curve varies.
KV Cyg Min II 11.9.
KY Cyg H2O, OH maser.
LN Cyg Min II 14.3.
LO Cyg Min II 13.3.
LX Cyg P var. Max = 2432775 + 460.0d*E (JD2415000 - 33300)
[1159]; since JD2437900 - see
Table. SC 7/9-e - SC 8/8.5e.
MQ Cyg VB A (B 17.5m B, 4.5", 122deg). P var. Max = 2432737 +
+ 428.5d*E (JD2414300 - 33300) [1229]; since
JD2440000 - see Table.
MR Cyg Min II 9.12; d = 0.030P; DII = 0.19P.
MU Cyg Min II 14.4.
MY Cyg Min II 8.99. Min II - Min I = 0.5021P.
MZ Cyg P var. Max = 2427641.914 + 21.162460d*E + 0.10575d*
*10**-3*E**2 (JD2414900 - 37900) [3689]; since
JD2443600 - see Table.
Probably it is
an RV Tau type variable, and then the period should
be doubled [8862]. [A/H] = 0.1.
NQ Cyg EW type
is possible. Close to V736 Cyg.
NU Cyg Min II 14.9.
NZ Cyg Min II 14.2.
OS Cyg P var.
OU Cyg Min II 15.6.
OY Cyg Star 23 - 30 [1321].
PP Cyg Star G in the
chart for VV245 [7749].
PR Cyg Star 24 - 40 [1321].
PT Cyg Star 23 - 55 [1321].
PU Cyg Star 25 - 56 [1321].
PX Cyg Star 35 - 78 [1321].
PY Cyg Min II 15.2.
QS Cyg Min II 13.3.
QT Cyg Depth of Min II 0.04m.
QU Cyg Min II 15.1.
QW Cyg Min II 14.1.
QX Cyg Min II 14.5.
V339 Cyg np component of a
close binary.
V340 Cyg Min II 14.5.
V343 Cyg [A/H] = -0.2.
V346 Cyg Companion 13.8m, 0.4' sf. Min II 11.9. P var.
Min I = 2427270.241 + 2.743345d*E (JD2415000 - 32000);
since JD2432000 - see Table.
V348 Cyg According to [7516] EW type va-
riable with large irregularities: Min = 2441567.177 +
+ 0.285768d*E (JD2441567 - 95).
V355 Cyg Min II 14.3.
V360 Cyg P var [6107]. Min I = 2429187.4 + 70.449d*E (JD
2414600 - 34000) [0580]; since JD2426000 -
see Table.
V366 Cyg Min II 10.2.
V367 Cyg VB A (A 0.1", 50deg; B 13.7m, 2.3", 255deg). Min II 7.16.
Shape of the light curve and the radial velocity curve
vary.
V368 Cyg According to [0204] EB type (12.8m - 13.8m pg)
with the elements: Min I = 2425808.10 + 0.47586d*E
(JD2425805 - 853).
V369 Cyg P var. Max = 2438199 + 104.46d*E (JD2426000 - 38200);
since JD2438200 - see Table.
V370 Cyg Min II 11.9. P var. Min I = 2425096.429 + 0.77453979d*E
(JD2414400 - 30000); since JD2430000 -
see Table.
V371 Cyg Min II 12.5.
V374 Cyg d = 0.03P.
V380 Cyg Min II 5.76; Min II - Min I = 0.418P (1963).
There are periodic
terms in the elements: + 0.8916d sin (38.8deg + 0.0082deg*E) -
- 0.0796d sin (77.6deg + 0.0164deg*E) + 0.0088d cos (26.4deg +
+ 0.0246deg*E); Min II = 2441262.266 + 12.425612d*E -
- 0.8916d sin (38.8deg + 0.0082deg*E) - 0.0796d sin (77.6deg +
+ 0.164deg*E) - 0.0088d cos (26.4deg + 0.0246deg*E).
Apsidal motion is possible with P = 1490 years.
V382 Cyg VB A (B 11.5m, 11", 332deg). Min II 9.12.
Shape of the
light curve and depth of Min II vary. P var. Min I =
= 2427992.458 + 1.885497d*E (JD2413480 - 29500)
[1253]; since JD2428000 - see
Table.
V385 Cyg Min II 12.4.
V387 Cyg Min II 11.6.
V388 Cyg Min II 9.15; d = 0.06P. P var. Min I = 2433584.540 +
+ 0.8590507d*E (JD2427600 - 37200); since
JD2437200 - see Table.
V389 Cyg VB A (B 8.0m, 3.4", 305deg, 1980). SB (P = 3.313168d);
Turns around the invisible third compa-
nion with P = 154.09d.
According to [1256] the light varies with
two alternate periods P1 and P2. The first oscillation
(P1) with A = 0.19m satisfies the elements: Max =
= 2423298.460 + 1.12912d*E, the second (P2) with A =
= 0.05m - the elements: Max = 2429162.080 + 1.19328d*E.
each of them continues for 1 - 3 weeks. At the transi-
tion from one oscillation to the other irregular light
variations are sometimes observed or almost constant
brightness. At the renewal of each oscillation its phase
remains unchanged, experiencing no shift. According
to [8909] in 1975 - 1977 periodicity was not observed.
V393 Cyg d = 0.02P.
V401 Cyg Min II 11.13. P var. Min I = 2432881.277 + 0.582717d*E
(JD2428800 - 34000); since JD2434000 -
see Table.
V402 Cyg VB A (B 20", 90deg).
V407 Cyg VB A (B 14.0m, 8", 190deg).
Light variations of the Mira type
variable are superimposed by the outburst of the pro-
bable nova which occured near JD2428400 (1936)
with the consequent slow light decrease. Combined
spectrum.
V411 Cyg P var. Max = 2421075 + 321d*E (JD2421000 - 31100)
[1262]; since JD2431100 - see
Table.
V416 Cyg Red.
V425 Cyg Des-
cription of the spectrum and its variations [2685, 3149].
V427 Cyg P var. Max = 2425471 + 143d*E (JD2425400 - 5950)
[1155]; since JD2433850 - see
Table.
V429 Cyg In the region of the
open cluster NGC 6883.
V430 Cyg See V429 Cyg. Max = 2425544 + 258d*E (JD
2425500 - 27400) [1155].
V432 Cyg In the
region of the open cluster Dolidze 3.
V439 Cyg In the region of
the open cluster Berkeley 87 = OCL 161.
V441 Cyg Epoch of Min I is given.
V442 Cyg Min II 10.4:, d = 0.01P:.
According to
[8721] the period given in [0525] must be doubled.
V443 Cyg There is a periodic term in the elements:
-0.016d sin 0.00105*E.
V444 Cyg In the H II region S 109. Min II 8.06;
D II = 0.10P. P var. Min I = 2430856.453 + 4.21238d*E (JD
2415000 - 30000) [0007]; since JD2430000 -
see Table.
V445 Cyg P var. Min = 2425527.391 + 1.947833d*E (JD2425500 -
34700) [1155]; since JD2434700 -
see Table.
V447 Cyg In the region of the
open cluster NGC 6871.
V448 Cyg See V447 Cyg. Min II 8.40.
V450 Cyg The light curve resembles that of DQ Her.
V453 Cyg See V447 Cyg. Min II 8.68; d = 0.03P; Min II - Min I =
= 0.5077P. [7518]
According to [7518] there is
Apsidal motion with P = 71 years.
V454 Cyg Min II 12.3. In the
region of the open cluster IC 4996.
V455 Cyg Min II 10.9. P var. Min I = 2431151.908 + 8.7689331d*E
(JD2426800 - 33950) [1286]; since JD2436800 -
see Table.
V456 Cyg Min II 11.4; Min II - Min I = 0.518P. P var?
V457 Cyg Min II 13.9.
V458 Cyg Min II 14.2.
V461 Cyg PB ~ 7000d? [8251].
V462 Cyg P var. Max = 2428540 + 376.0d*E (JD2416000 - 35200);
since JD2435200 - see Table.
V463 Cyg Min II 10.65; Min II - Min I = 0.514P.
V465 Cyg There is a close com-
panion of 17.5m.
V466 Cyg Min II 11.4.
V469 Cyg Min II 12.9; Min II - Min I = 0.57P.
V470 Cyg Min II 8.545.
V471 Cyg S 5.5/5.5.
V473 Cyg P var. Max = 2430615 + 218.5d*E (JD2418000 - 31000)
[0346]; since JD2442300 - see Table.
V474 Cyg d = 0.014P.
V477 Cyg Min II 8.69; D II = 0.09P; d = 0.003P. P var. Min I =
= 2429194.309 + 2.3470011d*E (JD2410000 - 29200)
[0001]; Min I = 2437317.2695 + 2.3469943d*E (JD
2429200 - 39700) [8919]; since JD2439700 -
see Table.
Apsidal motion
with Pi = 349 years; E = 0.302 [6175]. 0.331P (1965 - 1970) <=
<= Min II - Min I < = 0.460P (1904).
V478 Cyg VB A (B 12.8m, 4", 259deg. Min II 9.02; Min II - Min I =
= 0.5072P.
V482 Cyg VB A (B 14.4m V, M4 III, 8", 225deg).
V483 Cyg Min II 11.9.
V484 Cyg Min II 13.6.
V486 Cyg Min II 14.3.
V488 Cyg Min II 13.0.
V490 Cyg Min II 13.5; Min II - Min I = 0.47P.
V491 Cyg Min II 14.7.
V493 Cyg Min II 12.9.
V494 Cyg Min II 13.6.
V496 Cyg Min II 12.5.
V498 Cyg Min II 10.27.
V500 Cyg VB B (A 11.5m; 18", 45deg). Min II 12.0.
V501 Cyg Min II 13.1; d = 0.02P.
V502 Cyg Min II 14.2.
V505 Cyg Min II 12.0.
V509 Cyg d = 0.05P.
V512 Cyg Min II 11.5.
There is a periodic term in the elements: +0.065d*
*sin 0.2105263deg (E + 538).
V513 Cyg Min II 12.6.
V519 Cyg Min II 13.4.
V520 Cyg VB A (B 15", 135deg).
V525 Cyg d = 0.03P:.
V526 Cyg Min II 13.1. In the
region of the open cluster TGC 7039.
V532 Cyg P var. Max = 2434618.158 + 3.283651d*E (JD2427900 -
35000); Max = 2436817.694 + 3.282792d*E (JD2435000 -
38700); since JD2438700 - see
Table.
V536 Cyg d = 0.010P.
V538 Cyg B - V: +1.17, +1.50.
V539 Cyg P2 = 1500d.
V541 Cyg Min II 10.9; DII = 0.012P; Min II - Min I = 0.453P.
V544 Cyg P var?
V546 Cyg Min II 15.2:; Min II - Min I = 0.48P; d = 0.077P.
In the dark nebula Barnard 144.
V547 Cyg B - V: +1.27, +1.73. In the dark
nebula Barnard 144.
V548 Cyg Min II 8.62. P var. Min I = 2442279.3838 + 1.80524695d*E
(JD2430800 - 42300) [8930]; since JD2442300 -
see Table.
V563 Cyg P var. Max = 2427590 + 295.4d*E (JD2426000 - 30250);
since JD2430250 - see Table.
V567 Cyg d = 0.036P.
V581 Cyg Red.
V586 Cyg In the region of the
open cluster NGC 7039.
V588 Cyg VB A (B 18m, 15", 0deg). Very Red.
V589 Cyg VB.
V606 Cyg P var. Max = 2428376.7 + 50.245d*E (JD2427950 -
31330) [1262]; since JD2437100 -
see Table.
V612 Cyg Cycles of 50 - 100d (JD2427950 - 31330) [1262];
since JD2437100 - see Table.
V614 Cyg Min II 14.5.
V618 Cyg In the region of the
open cluster TGC 7092.
V622 Cyg see V618 Cyg.
V628 Cyg Min II 12.5.
V635 Cyg Min II 13.5.
V643 Cyg P var. Elements given in the
Table are valid in the interval JD2427950 - 31330.
V644 Cyg VB A (B 15.6m, 6", 141deg; C 16.3m, 6", 141deg).
V645 Cyg Observed as the
bright nebular condensation with ~ 2" diameter scat-
tering light of an O8 star associated with it but invi-
sible because of absorption. A part of strongly polari-
zed bipolar nebula with diameter about 10". There are
strong emission lines of H, Fe II, [O I], [S II], etc. In
the spectrum [8942, 9129]. H2O maser source. Infra-
red source CRL 2789.
V651 Cyg Min II 14.7.
V652 Cyg Min II 12.1.
V664 Cyg d = 0.05P.
V666 Cyg P var. Max = 2427965 + 236d*E (JD2427950 - 31350)
[1262]; since JD2433400 - see
Table.
V670 Cyg sp component of a close binary.
V680 Cyg Min II 10.3.
V685 Cyg VB.
V687 Cyg Min II 10.4. P var?
V688 Cyg d = 0.029P.
V690 Cyg d = 0.021P.
V691 Cyg d <= 0.034P.
V692 Cyg Min II 14.9?
V693 Cyg Min II 14.4?
V694 Cyg d = 0.017P.
V695 Cyg 31 Cyg.
Probably enters a common system
with V1488 Cyg (32 Cyg).
VB A (B 13.0m, 36.8", 332deg; C 6.99m, 107.0", 174deg; D 5.0m,
338", 323deg). d = 0.0151P.
Interferometric binary eclipsing system (A = 0.08", E = 0.15
[1582]; 0.035", 141.8deg, 1980.4). The epoch of eclipse of
the component of the spectral type B4 by the compo-
nent of the type K4 is given in the Table. The ampli-
tude strongly varies depending upon the wavelength:
A(lambda 6560 A) = 0.03m, A(lambda 3530 A) = 1.80m [9131].
V696 Cyg Mean magnitude varies with P = 1600d.
V700 Cyg Min II 12.3. P var. Min I = 2432028.863 + 0.340047d*E
(JD2431700 - 37500) [5352]; since JD
2437500 - see Table.
V704 Cyg Min II 14.2.
V706 Cyg Min II 13.9.
V713 Cyg Min II 15.1.
V720 Cyg P var. Min I = 2427611 + 332d*E (JD2429450 - 32000)
[0798]; since JD2432500 - see
Table.
V726 Cyg Min II 12.8; d = 0.018P.
V728 Cyg P var. Min = 2425760.475 + 2.0601256d*E (JD2425500 -
35000) [0164]; since JD2439700 -
see Table.
V729 Cyg VB A (B 13.5m, 1.5", 65deg). Min II 9.29. P var. Min I =
= 2434264.638 + 6.597700d*E (JD2428700 - 37900)
[0001]; since JD2439750 - see
Table.
V731 Cyg VB.
V735 Cyg Depth of Min II 0.04m.
V736 Cyg Min II 16.5. Close to NQ Cyg.
V737 Cyg Star 23 - 50 [1321].
V739 Cyg Star 36 - 81 [1321].
V741 Cyg d = 0.03P.
V742 Cyg P var. Max = 2429409.448 + 0.93979d*E (JD2428420 -
30700) [8977]; Max = 2431489.580 + 0.94010d*E (JD
2430250 - 32350); Max = 2433282.014 + 0.93979d*E (JD
2432350 - 33650); since JD2433650 -
See Table. According to [8977]
since JD2430700 the observations are better repre-
sented by the elements: Max = 2432943.701 + 0.93977897d*E -
- 1.067d*10**-7*E**2.
V747 Cyg The intervals between maxima of brightness
are 2000 - 4000d. Not red.
V751 Cyg In the region of the nebula
IC 5070. SB (P = 0.25d [9132]).
Rapid small
variations near maximum of brightness ( = +0.25)
are superimposed sometimes by deep minima lasting
for some hundreds days [2699]. Soft X-ray source
[9133]. Spectrum description [2698, 9132].
V752 Cyg = +0.77, = -0.47.
V753 Cyg d = 0.12P. P = 0.952374d?
V757 Cyg Red.
V758 Cyg P = 400d?
V759 Cyg P var. Max = 2434513.427 + 0.36001476d*E (JD
2414430 - 34570) [3506]; since JD2434500 -
see Table.
Blazhko effect.
V779 Cyg Type RR?
V781 Cyg P var?
V783 Cyg P var. Max = 2433261.029 + 0.62069487d*E (JD2424690 -
34000); since JD2438970 - see
Table.
V786 Cyg Usually in minimum brightness, with rapid
brightenings by 0.5m - 1.0m. In the interval JD2427692 -
697 the brightness was 13.5m.
V789 Cyg P var? [Fe/H] = -0.91.
V795 Cyg sf component of a close
pair.
V796 Cyg Min II 11.4.
V797 Cyg Min 15.4.
V799 Cyg P var.
V801 Cyg There is a
square term in the elements: +1.93d*10**-10*E**2.
V802 Cyg P var. Max = 2432779.9342 + 0.59560377d*E (JD
2425480 - 35170) [2775]; Max = 2439415.263 +
+ 0.5955638d*E (JD2435950 - 40000) [9266]. Max =
= 2440036.409 + 0.595447d*E (JD2440000 - 41000); Max =
= 2441517.498 + 0.595635d*E (JD2441000 - 42500);
since JD2442500 - see Table.
Shape of the light curve
varies (0.13P <= M - m <= 0.50P); period variations are accom -
panied sometimes by strong variations of amplitude (in
the interval JD2440000 - 41000; 0.3m <= A <= 1.7m).
V803 Cyg Min II 14.5.
V806 Cyg Min II 15.0; DII = 0.061P.
V807 Cyg Min II 14.9.
V808 Cyg Brightness in maximum
varies.
V809 Cyg Min II 13.6; DII = 0.069P.
V810 Cyg d = 0.050P. Depth of Min II 0.05m. P var?
V817 Cyg sp component of the pair.
V818 Cyg Shape of
the light curve and period vary.
V821 Cyg Min II 15.6.
V822 Cyg Min II 13.0.
V824 Cyg Min II 14.3.
V825 Cyg Min II 16.9. Min II = 2433871.915 + 7.709015d*E.
V826 Cyg Min II 14.7.
V828 Cyg Min II 10.12.
V832 Cyg VB A (B 9.43m, 20", 352deg; C 11.62m, 27", 141deg; D 12.72m,
38", 220deg). descrip-
tion of spectral variations [9135].
V836 Cyg Min II 8.77. P var. Min I = 2426547.5224 + 0.65341090d*E
(JD2425500 - 42000) [3869]; since JD
2441200 - see Table.
Shape of the light
curve varies.
V840 Cyg LS II 28.3deg [8090]. Cycles 250 - 300d.
V841 Cyg Min II 11.2.
V842 Cyg Min II 14.1.
V844 Cyg VB A (B 17.8m, 2.9", 50deg).
V850 Cyg Min II 11.8. P var. Min I = 2430587.263 + 4.5578d*E (JD
2428750 - 30590) [4253]; since JD2434330 -
see Table.
V851 Cyg d = 0.017P?
V852 Cyg Min II 14.9.
V853 Cyg Min II 14.2.
V856 Cyg Depth of Min II 0.05m.
V857 Cyg Depth of Min II 0.03m.
V859 Cyg Min II 12.1.
V865 Cyg Min II 14.6.
V866 Cyg Min II 13.9.
V869 Cyg Min II 14.8. Shape
of the light curve varies.
V870 Cyg Min II 15.8.
V871 Cyg Min II 14.9.
V873 Cyg Min II 14.7. Min II - Min I = 0.48P.
V874 Cyg Min II 13.8.
V877 Cyg Min II 12.9.
V880 Cyg Min II 14.1; Min II - Min I = 0.506P; d = 0.02P.
V881 Cyg delta(S) is small [9037].
V882 Cyg [Fe/H] = -1.42.
V884 Cyg np component of a pair. Min II
14.2.
V885 Cyg Min II 10.2.
V886 Cyg Min II 14.1; Min II - Min I = 0.515P.
V887 Cyg Depth of Min II 0.03m.
V888 Cyg Min II 15.9.
V889 Cyg Min II 10.4.
V891 Cyg Min II 9.4.
V892 Cyg Min II 15.5. nf compo-
nent of a close pair.
V900 Cyg Min II 15.2.
V902 Cyg d = 0.02P. Depth of Min II 0.05m.
V906 Cyg Min II 15.7.
V907 Cyg Min II 14.9. According to [4427] Min I =
= 2435066.257 + 0.54138554d*E.
V908 Cyg nf component of a close pair. Depth of Min II 0.04m.
V909 Cyg Min II 9.66.
V910 Cyg Min II 14.2; d = 0.02P.
V911 Cyg Min II 14.6. P var? Min I = 2432120.251 + 3.42262215d*E
(JD2415500 - 37900) [4761]; since JD
2437100 - see Table.
V912 Cyg Depth of Min II 0.05m.
V913 Cyg VB A (B 17m, 0deg).
V920 Cyg A var. Blazhko effect?
V922 Cyg d = 0.02P:.
V924 Cyg P var. Max = 2435706.776 + 5.5709816d*E (JD2432760 -
38000) [8053]; since JD2438000 -
see Table.
V925 Cyg Min II 16.0.
V927 Cyg Epoch of Min brightness is
given.
V928 Cyg Min II 15.4.
V931 Cyg Min II 14.5.
V932 Cyg Depth of Min II 0.04m.
V934 Cyg Min II 13.7.
V936 Cyg Depth of Min II 0.05m.
V939 Cyg Min II 12.5.
V940 Cyg Min II 15.1.
V941 Cyg Min II 13.2.
V942 Cyg VB A (B ~ 10deg, C ~ 110deg).
V944 Cyg np component of pair.
V947 Cyg Min II 15.0.
V948 Cyg Min II 15.2.
V949 Cyg Red.
V955 Cyg Min II 15.3. sp compo-
nent of a close pair.
V956 Cyg Min II 15.1. sp compo-
nent of a close pair.
V957 Cyg Min II 12.6.
V958 Cyg P = 199d?
V959 Cyg Min II 11.4; Min II - Min I = 0.52P; DII = 0.16P:.
sp component of a close
pair.
V961 Cyg Min II 12.4; Min II - Min I = 0.505P.
V962 Cyg d = 0.02P:.
V964 Cyg Min II 14.4.
V965 Cyg Min II 14.9. Type RRC? P = 0.32028628d?
V970 Cyg Min II 14.8.
V974 Cyg Min II 12.5; Min II - Min I = 0.462P. Min II = 2435373.398 +
+ 3.204418d*E.
V979 Cyg Min II 14.7.
V981 Cyg Min II 15.0.
V997 Cyg [Fe/H] = -0.77.
V997 Cyg [Fe/H] = -0.77.
V1004 Cyg Min II 13.0.
V1007 Cyg See V932 Cyg.
V1008 Cyg Min II 16.0.
V1010 Cyg Depth of Min II 0.03m.
V1011 Cyg See V932 Cyg.
V1012 Cyg Min II 15.4.
V1016 Cyg Before the outburst in 1964 the brightness
changed between 15.0m and 17.5m pg [5701], the spect-
ral type was late Me alfa [1222]. In the 1964 - 67 the
brightness increased from 16.0m to 11.2m B. In 1967 -
69 the brightness steadily increased to 10.05m B,
being constant in V system (10.5m). In the infrared it
changes in the limits 6.9 - 8.4 J, 4.7 - 5.8 K with the
period 470d [7174, 9141]. High excitation emission
spectrum with strong IR excess resembles that of
symbiotic variables [9142]. X-ray and radio source.
V1018 Cyg Min II 11.6.
V1021 Cyg Min II 14.3.
V1023 Cyg Min II 12.9; d = 0.03P:. DII = 0.14P. Min II - Min I = 0.495P.
V1024 Cyg See V932 Cyg.
V1030 Cyg Elements given in the
Table are valid in the interval JD2426600 - 32300.
V1033 Cyg P var.
V1034 Cyg Min II 9.9.
V1035 Cyg P var?
V1037 Cyg Min II 14.8.
V1038 Cyg VB B (9.4", 215deg, 1963). Min II 15.5.
V1039 Cyg Min II 15.6.
V1042 Cyg VB A (B 10m, 53", 110deg). In HII re-
gion S 109.
V1044 Cyg Min II 16.5.
V1045 Cyg Min II 16.0.
V1047 Cyg d = 0.02P.
V1053 Cyg d = 0.05P.
V1057 Cyg In the dark nebula, in the region of the North America
nebula (NGC 7000). In 1969 - 70 (JD2440400 - 830)
the outburst from 16.5m to 10.3m occured. Brightness
maximum was observed at JD2440830 (spectrum-
B3). Before the outburst the light changed in the range
15.5m - 16.5m, the spectral type was Ke with characte-
ristic features of T Tau type stars [2698, 6415]. Af-
ter the outburst the brightness began to weaken mo-
notonouosly and in 1982 reached 13.1m B (the spect-
ral type about G2 - G5 Ib). Strong H alfa emission appea-
red in 1971. There are also small rapid light fluctua-
tions. Description of light variations [6504, 7115,
7754, 8996]. The star is associated with a luminous
arc-shaped reflection nebula. This nebula with length
of about 3' appeared in 1971 and its brightness is
gradually decreasing simultaneously with the fading
of the star.
V1061 Cyg Min II 9.5.
V1063 Cyg P var. Max = 2428260 + 339d*E (JD2428260 - 30700);
since JD2433500 - see Table.
V1064 Cyg Min II 15.3.
V1068 Cyg Min II 11.2; d = 0.070P.
A migrating wavelike distorsion with
an amplitude ~ 0.1m V is being observed outside ec-
lipses [8999].
V1073 Cyg Min II 8.57.
V1074 Cyg Min II 14.8.
V1083 Cyg Min II 11.2.
V1085 Cyg Observations given in
[7010] contradict the elements given in [7193]: Min =
= 2437856.592 + 2.8089d*E.
V1096 Cyg d = 0.03P.
V1102 Cyg Radio-quiet N ga-
laxy. Absorption spectrum without emission lines;
z = 0.0272.
V1111 Cyg Blazhko effect is pos-
sible.
V1122 Cyg See V1111 Cyg.
V1130 Cyg Min II 12.9.
V1136 Cyg Min II 13.2.
Eccentric orbit (E =
= 0.3). Apsidal motion is possible [8051].
V1141 Cyg Min II 11.8.
V1142 Cyg Min II 13.4.
V1143 Cyg Min II 6.06; Min II - Min I = 0.743P; d = 0.002P.
V1157 Cyg Min II 13.6.
V1158 Cyg d = 0.02P; See V932 Cyg.
V1161 Cyg d = 0.01P.
V1162 Cyg Only one Max was observed
(See Table). Thereafter - either invisible, or fairly
constant (17.6m - 17.8m). Bluish.
V1171 Cyg VB A (B 11.0m, 0.34", 71.2deg; 1979.5). Min II 10.3.
V1175 Cyg Min II 16.5. P var. Min I = 2434629.545 + 1.3330d*E
(JD2426620 - 34630); since JD2434635 -
see Table.
V1176 Cyg VB. Variable is probably the
northern red component.
V1187 Cyg In the nebula IC 1318B. Min II 11.19.
P = 3.7675d?
V1188 Cyg Min II 14.3.
V1189 Cyg Min II 13.7. P var. Min I = 2437906.516 + 1.041908d*E
(JD2426620 - 31240); since JD2437906 -
See Table.
V1191 Cyg In the nebula IC 1318B. VB A (B 13m,
11", 299deg; C 13m, 11", 284deg). Min II 11.11.
Shape of the light
curve varies.
V1193 Cyg Min II 14.3.
V1196 Cyg See V936 Cyg.
V1200 Cyg Min II 16.1:.
V1210 Cyg Red.
V1212 Cyg See V1210 Cyg.
V1218 Cyg VB A (B 17m, sf).
V1225 Cyg VB A (B 16m V, B - V = +1.3m, 1.2", 270deg; C 15.0m V,
B - V = +0.5m, 2.4", 270deg); P var? Max = 2428250 +
+ 384.2d*E (JD2428200 - 38250) [3160]; since
JD2438500 - see Table.
V1236 Cyg Red.
V1255 Cyg Brightness in Max varies in
the range 15.2m - 16.0m with possible elements: Max =
= 2439382.281 + 0.28619537d*E.
V1256 Cyg Min II 14.1.
V1273 Cyg Min II 16.5.
V1275 Cyg In the region of the
open cluster NGC 6819.
V1281 Cyg Min II 15.4.
V1285 Cyg Red.
V1302 Cyg See V936 Cyg.
V1305 Cyg Min II 11.5m - 11.7m (var).
V1307 Cyg Considerable dispersion of mean light curve
points.
V1315 Cyg Min II 15.3.
V1316 Cyg (P) > 100d.
V1318 Cyg LkH alfa 225. See V1331 Cyg.
V1321 Cyg P = 0.7281802d?
V1322 Cyg In the region of
the open cluster NGC 6913.
V1326 Cyg Min II 11.8; Min II - Min I = 0.53P.
V1327 Cyg Very red.
V1329 Cyg In 1891 - 1964
light variations in the range 14.2m - 15.5m with deep
minima to 18m; the minima are satisfied by the ele-
ments given in the Table; D = 0.1p; spectral type M
[7235]. In 1964 - the outburst up to 12.1m. Then gra-
dual brightness decrease superimposed by periodical
variations with an amplitude near 1m. Light minima
as before are satisfied by the elements given in the
Table but the character of eclipses changed (probably
because of appearance of a dense envelope ejected
by one of the components of the system). After the
outburst high excitation emission spectrum with IR
excess is observed similar to the spectrum of sym -
biotic variables.
V1331 Cyg Associa-
ted with a cometary nebula.
V1334 Cyg VB A (B 7.9m, B5 - B8, 0.13", 26.1deg, 1975).
V1336 Cyg According to [7010], RR? P = 0.5d?
V1341 Cyg Cyg X-2. SB 1. Halo
object (nu = -220 km/s). Strong reflection effect changes
the spectral type of the F component. Spectral line pro -
files vary. The lines of He II, KCa II, C III,and N III are
in emission. The system has low and high states. Du-
ring the low state the mean light curve is a double
wave with the range 15.1m - 15.4m B. Epoch of Min I gi -
ven in the Table corresponds to the F star in supe-
rior conjunction; Min II 15.4. The eclipse of the ac-
cretion disk at the phase 0.5P in partial. Rapid light
variability by 0.1m in 10 minutes and by 0.5m in seve -
ral hours is superimposed. In the high states lasting
for ~ 10d the mean light increases by 0.5m. Radio
source at 8085 MHz, source of soft and hard X-ray
emission from 0.1 to 60 KeV.
V1345 Cyg Min II 15.0:.
V1354 Cyg See V932 Cyg.
V1356 Cyg Min II 10.4.
V1357 Cyg Cyg X-1. SB1.
The epoch of the inferior
conjunction of the optical component is given in the
Table. Min II 8.88. The shape of the light curve va-
ries; Min II sometimes are not observed. The perio-
dicity in the light curve variations as well as in po-
larization changes is possible with P = 78.4d [9021,
9022]. Rapidly variable X-ray source in wide range
up to 3 MeV characterized by the change of high and
low states. Light and X-ray variation with P = 294d
is also detected [9154, 9156]. Variable and flare ra -
dio source at 2695 and 8085 MHz.
V1372 Cyg P2 = 360d?.
V1374 Cyg Min II 17.7.
V1384 Cyg In the region of
the open cluster NGC 6913.
V1396 Cyg VB AB (10.26m V, 12.3m V; A = 0.1127", P = 29.33 Y
[9026]); mu = 0.67", P = 113deg; A-SB 2 (mAb - mAa = 0.6m,
P = 3.275631d [9025]).
Probably all the three com-
ponents of the system are variables of the UV Cet
type, and according to [5716] also of the BY Dra
type. The range of combined brightness of the system
is given in the Table. Really the flare of AB compo -
nent was observed in the spectrograms [9025].
V1401 Cyg Min II 13.6.
V1410 Cyg P > 400d.
V1411 Cyg P = 1.553478d?
V1412 Cyg Min II 15.5.
V1414 Cyg Northern compo-
nent of a close pair; d = 0.04P.
V1416 Cyg Min II 14.7.
V1417 Cyg Min II 13.1.
V1421 Cyg In the region
of the planetary nebula NGC 6857 = K3 - 50.
V1425 Cyg Depth of Min II 0.31m.
V1427 Cyg In the region of
the open cluster M39.
V1429 Cyg Min II 15.3.
V1430 Cyg Min II 15.0.
V1436 Cyg Min II 15.9, D II = 0.08P; Min II - Min I = 0.48P.
V1437 Cyg Min II 16.0.
V1440 Cyg In the region of
the open cluster NGC 6819.
V1465 Cyg Resembles an eclipsing va-
riable.
V1478 Cyg VB A (B 17m:, 3", 80deg).
Compact radio source. extended structure cen -
tered at the star is observed at 5 Ghz. Bq [] star
with the excess of infrared radiation of dust at T =
= 300degK. Description of the spectrum [7080, 7081, 7523,
9159, 9160].
V1479 Cyg In the region of the nebula
IC 5070.
V1481 Cyg Min II 12.5. In the region of the open cluster NGC 7128.
V1485 Cyg Brightness in Max
strongly varies.
V1488 Cyg 32 Cyg. Probably enters a common sy-
stem with V695 Cyg (31 Cyg).
0 < d < 0.011P. P var. Min I = 2420670.0 + 1140.1d*E (JD
2411400 - 29700). Since JD2429700 -
see Table.
The epoch of the eclipse of the B4 type
Component by the K5 type component is given. There
is also small physical light variability of the K com-
ponent [8896, 9161]. Depth of eclipses depends of lambda:
0.04M V, 0.13m B, 0.27m (lambda 4243A),0.90m (lambda 3552A).
V1489 Cyg NML Cyg. 17.0m: - 18.0m V, B>21M; I - K = + 8.17.
Very large IR exess due to expanding ga-
seous-dust envelope. In the area 2.5"*3.5" around
the star the system of about 60 discrete sources of
OH emission is detected [7461]; source of OH, H2O,
SiO maser emission. Light variations are periodical
(see also [9163]). The object may be a protostar being
observed at the end of condensation process. The late
spectrum arises probably in the extending envelope
[9165, 9166].
V1490- V1492 Cyg
See V1479 Cyg.
V1493 Cyg See V1479 Cyg. V1707 Cyg 10.5"P.
V1494 Cyg See V1479 Cyg.
V1495 Cyg In the region of the nebula
NGC 7000.
V1497 Cyg See V1495 Cyg.
V1498 Cyg See V1495 Cyg.
V1500 Cyg In August 1983, before the very rapid increase
of light, the brightness of the Nova gradually increased
from 17.6m to 13.5m B (JD2442632 - 653.2). After Max
almost monotonous decay of brightness is superimpo -
sed by light variations with the amplitude of 0.03m -
1.0m V; the period of these variations in the interval
JD2442656 - 43100 changed in the range 0.1415d [9167,
9168] - 0.137d [9169, 9170]. Since JD2443100 Min =
= 2443696.4827 + 0.1396133d*E. Some investigators (see,
for instance, [9173]) adopt double value of this pe -
iod. A month after the light maximum of the Nova the
radio emission was registered at 2695 and 8085 MHz
[9171].
V1507 Cyg The epoch of a broad Min I (superior conjunction of
the B component) is given; Min II 7.01; D II = 0.20P,
Min II - Min I = 0.29P; e = 0.39. Unusual light curve
[8213, 9049]. Shape of the light curve and depths of
Min vary. Gaseous streams And expAnding envelope.
V1508 Cyg Min II 13.3.
V1509 Cyg VB A (B 11.7m, 55", 106deg).
V1511 Cyg V - K = 13.6m.
V1513 Cyg Gliese 781; mu alfa = -0.146S, mu delta = -1.00"; SB.
V1515 Cyg In a dark nebula, near the nebula
NGC 6914. Connected with nebular appendage like a
Comma. Light increase was observed from 1944 till
1958. Since 1958 the star is in Max. Slow light varia-
tions with A <= 1.6m. The absorption line Li I lambda 6707A
is seen in the spectrum.
V1521 Cyg Cyg X-3. Peculiar infrared X-ray source. V > 23m.
Flare radio source. In the K band short and slow fla-
res on the time scale about 2 minutes and 1 - 2 hours,
irregular variations and longperiodic variability are
observed [7752]. These variations are accompanied
by periodical oscillations of infrared, X-ray and gamma
radiation with the elements: Min = 2440949.8986 +
+ 0.1996830d*E + 1.25d*10**-10*E**2 [9187]. Usually the
amplitude of these variations A(K) = 0.5m, but some -
times they disappear completely.
V1523 Cyg Amplitude and mean brightness strongly vary.
V1531 Cyg LkH alfa 142. VB A (B = V1532 Cyg, 2.5", 90deg). See
V1479 Cyg. Combined
brightness and spectrum are given.
V1532 Cyg LkH alfa 143. VB B (A = V1531 Cyg; B 2.5", 90deg).
See V1531 Cyg.
V1535 Cyg See V1479 Cyg.
V1536 Cyg See V1495 Cyg.
V1538 Cyg See V1495 Cyg.
V1539 Cyg See V1495 Cyg.
V1540 Cyg See V1495 Cyg.
V1546 Cyg See V1495 Cyg.
V1548 Cyg VB A (B 16.7m, 6.2", 131deg).
V1554 Cyg VB A (B 14.7m, 3.5", 214deg).
V1577 Cyg In the cluster and nebula
IC 5146.
V1578 Cyg See V1577 Cyg. VB A (B 15m, 5", 45deg; C 17m,
5", 225deg).
Associated with a reflecting nebula.
V1580 Cyg There
is a periodic term in the elements: - 0.027d sin 0.045deg
(JD - 2439000).
V1581 Cyg G 208 - 44. VB A (B = G 208 - 45, 15.97m V, M6Ve; 7.9",
106deg, 1954; 8.2", 96deg, 1974). mu = 0.71", P = 140deg.
The flare was observed during spectro-
scopic observations [9175]. The companion may be
also a UV Cet type variable. The range of combined
brightness variation of the system is given.
V1584 Cyg Epoch of min brightness is
given.
V1597 Cyg See V1479 Cyg.
V1598 Cyg See V1479 Cyg.
V1600 Cyg See V1479 Cyg.
V1608 Cyg See V1495 Cyg.
V1610 Cyg Infrared source
CRL 2688, the star of the spectral type F5Ia, associa -
ted with a bipolar reflection nebula (the so-called Egg
nebula). The northern component of the nebula is 4"
to the north from the source. Since 1920 to 1958 the
integrated light of this component increased from 15.2m
to 13.4b B and after that does not vary [8735]. Light
of the faint (16.2m B) southern component (5" to the
south from the source) varies by 0.6m B [9176]. The
radiation of the nebula is strongly polarized (46%,
teta = 106deg in V system). There are C3 absorption fea-
tures as well as Na, C2, and [S II] emission in the
spectrum. Probably the object is a precursor of a pla-
netary nebula [9178].
V1611 Cyg See V1495 Cyg.
V1624 Cyg A var.
In 1957 out of a B star
turned into Be star. Probably must be referred also
to GCAS type.
V1661 Cyg VB A (B 11.14m, 20", 174deg).
V1668 Cyg There are sinusoidal
light variations with A(V) = 0.15m and elements Min =
= 2443767.475 + 0.4392d*E in the descending branch
of the light curve after JD2443765 [9179]. Infrared
light curves (1.6 - 10 mkm) have a secondary maximum (JD
2443815) due to the formation of the dust envelope.
At 10 mkm this secondary maximum is brighter than the
primary one [9069].
V1669 Cyg d = 0.036P.
V1671 Cyg delta(U) = 0.06.
V1674 Cyg VB (B 15m, 5").
The range
of combined brightness variation is given. It is not
excluded that it is the component B that is variable.
SLow variations of mean brightness in the range
10.555m - 10.570m B are superimposed by sinusoidal pe-
riodikal ones with P1 = 1.3608d (A1 = 0.0037m) and P2 =
= 0.8055d (A2 = 0.0032m).
V1676 Cyg In the open cluster NGC 6871.
ADS 13374 A (B 12.0m, 6.5", 64deg; C 11.0m, 9.5", 28deg
D 9.5m, B3V, 11.4", 301deg; E 11.42m, 28.1", 109deg; F 7.36m,
B1IA, 35.9", 29deg); SB2 (P = 112.7d).
V1696 Cyg SB 1 (Porb = 4.3174d).
Epoch of Min brightness is given. The eclipse of the
accretion disc around the compact object formed in
the outburst of a Supernova in a binary system about
5*10**6 years ago is possible [3619].
V1701- V1704 Cyg
See V1479 Cyg.
V1706 Cyg See V1479 Cyg.
V1707 Cyg See V1479 Cyg. V1493 Cyg 10.5"f.
V1711 Cyg See V1495 Cyg.
V1716 Cyg See V1495 Cyg.
V1719 Cyg Shape of the light
curve varies.
V1720 Cyg Min II 7.79.
V1721 Cyg P var.Min I = 2442605.497 + 2.724370d*E (JD2442311 -
928); since JD2442928 - see
Table.
V1722 Cyg Min II 14.6?
V1726 Cyg Possible member of an anonimous open cluster.
V1727 Cyg 4U 2129 + 47. Lx/Lopt ~ 10.
Emissions in the spectrum: NeII lambda 4686A, CIII - NIII
lambda lambda 4640 - 50A.
V1735 Cyg In the complex of dark nebulae associated with the
open cluster and the nebula IC 5146. Lights up a
reflecting nebula. Became brighter by 5m at least
from 1952 to 1965.
V1737 Cyg B - V = +3.7.
V1738 Cyg B - V = +5.5:.
V1739 Cyg B - V = +4.5:.
V1744 Cyg Epoch of Max
in U system is given.
V1746 Cyg Sometimes P = 0.21d
is observed.
V1747 Cyg P > 100d. B - V = +4.0.
V1748 Cyg In the nebula IC 1318a.
V1751 Cyg In the nebula IC 1318c.
V1761 Cyg Close companion? Elements are not
certain.
alf Cyg VB A (B 11.4m, 75.3", 106deg).
tau Cyg VB A (B 6.44m, G1V, A = 0.88", P = 49.80yr; C 12.20m,
29", 230deg). 0.083d <= P <= 0.125d.
The range of total light
variation is given.
ips Cyg VB A (B 10.2m, 15.2", 220deg; C 10.2m, 21.5", 180deg).
hi Cyg VB A (B 10.8m, 158", 254deg). S 6 + %1e (Tc). SiO
maser. P var.Max = 2393559 + 405.88d*E (JD
2337150 - 94000); since JD2394000 -
see Table.
P Cyg The appearance of the star was firstly noted in
1600, when its brightness was 3m. Since the XVIII
century the light of the star varies in the range 4.6m -
5.6m vis. Radio source at the millimetre and centi -
metre wavelengths.
Q Cyg In minimum brightness varies
periodically with the amplitude 0.5m: Max = 2440495 +
+ 54.99d*E; P = 64.81d is also possible. Mean level of
brightness varies in the range 15.2m - 15.9m B.
S Del VB A (B 56", 342deg).
Double
maxima are sometimes observed.
U Del Mean brightness var, P = 1100d.
According to [8993], the period value 160d -
180d is more likely than 110d.
W Del d = 0.017P. Min II 9.79. P var. Since JD
2433000 - see Table.
The light curve shape var.
RZ Del VB (A var; B var, 17", 137deg) [3771].
TT Del P var. Since JD2435000 - see
Table.
TW Del delta(m) var (0.5m + 3.4m).
The light curve resembles that of
RV Tau, with Min I and Min II; the epoch of Min I is
given.
Min I = 2432171.1 + 118.4d*E (1947 - 1952); Min I =
= 2435386.8 + 115.9d*E (1955 - 1963); during
1964 - 1970 - see Table.
TX Del P var. P = 6.166585d (JD2428000 - 36600); since
JD2436600 - see Table.
TY Del Min II 9.8. P var.Min = 2428020.399 + 1.191121d*E (JD
2428000 - 38000) [0279]; since JD2438000 -
see Table.
TZ Del Epoch of Min is given.
VV Del Depth of Min II 0.05m.
YY Del Min II of the depth
~ 0.05m is possible.
P var. Min = 2425795.488 + 0.7930856d*E (JD2425000 -
34000) [1329]; since JD2434000 -
see Table.
AL Del Min II 12.4.
BG Del Min II 13.8.
BK Del P var?
BR Del Emission.
BX Del delta(S) = 0.
BY Del Min II 11.8.
CE Del [Fe/H] = -0.68.
CF Del The light curve shape var?
CH Del [Fe/H] = -1.23.
According to [9037], P = 0.315D.
CN Del Min II 14.6.
CR Del Min II 13.7.
CS Del [Fe/H] = -0.92.
CU Del Abrupt phase chande was noted.
CW Del P var.P = 0.58209d (JD ~ 2427100), P = 0.58211D (JD
~ 2428800); During JD2429800 - 30600 -
see Table.
DG Del The elements
should be checked.
DK Del Min II 14.2.
DM Del Min II 8.80.
DT Del Epoch od Min is given. The
elements are valid during JD2425480 - 6260.
DX Del [Fe/H] = - 0.11.
EG Del P var. Max = 2425535.42 + 0.3248545d*E (JD2425478 -
30619) [0911];
Abrupt change near JD
2432578, since then see Table.
EI Del The mean brightness var, P ~ 600d.
EK Del B - V: +0.29, +0.53.
ES Del Epoch of Max from [3715], [7527]
contradict the given elements.
ET Del Min II 12.7.
EW Del Min II 15.5.
EX Del Min II 13.3.
FL Del Min II 14.5.
FK Del Min II 14.5.
FM Del delta(S) = 0.
FP Del [Fe/H] = -1.44.
FR Del Min II 15.3.
FT Del Blazhko effect?
GG Del Min II 12.6. P var?
GN Del P var? delta(m) var?
GY Del VB B (A = BD +15deg 4134A, SP A - F).
HR Del Porb = 0.170920d. The brightness
began to increase on JD ~ 2439653. Waves with ma-
xima on JD2439752 (4.55m), 2439799 (4.64m), followed
by a sharp main Max, flat max on JD2439981 (4.09m)
and final decline. Radio source.
HU Del mu = 0.685", teta = 79deg.
Astrometric binary (semiamplitude of deviations
0.118", Porb = 1.52yr).
II Del [Fe/H] = -1.30.
IO Del A single outburst
was observed (JD2439378 - 388).
IV Del D ~ 0.1d.
LS Del Min II 8.76.
del Del (k - b)2 = 0.19. SB 2 (Porb = 40.58d; e = 0.7).
Spectra of both SB
components show Am features; Fe, Ca, Sc deficien-
cy, Sr, Y, Zr, Ba, Ce, La, Eu excess. Both compo-
nents are DSCT variables; the period of the main com-
ponent pulsation is 0.158d, that of the secondary is
0.134d [7528]. Any of the oscillations may occasio-
nally dominante in the combined brightness: according
to [7529], Max = 2439338.4444 + 0.135547d*E; accor-
ding to [7530], P = 0.154991d.
R Dor VB A (B 11.9m, 34", 10deg; C 11.0m, 35", 130deg, 1933).
H2O, SiO, HC3N emission.
S Dor VB A (B 12.1m, 13").
The member of the large magellanic
cloud. In the cluster NGC 1910 and a diffuse nebula.
One of the absolutely brightest stars. Deep Min: 1891,
1900, 1930, 1940, 1955, 1964.
T Dor VB A (B 12.0m vis, 5", 13deg.)
V Dor At the
edge of the Large Magellanic Cloud.
W Dor In the
region of the Large Magellanic Cloud.
X - Y Dor The member
of the Large Magellanic Cloud.
Z Dor See X Dor. In the nebula 30 Dor.
RR Dor See W Dor. Min II 14.5.
RS Dor See W Dor.
RU Dor See X Dor.
RW Dor See SW Dor. Min II 11.2.
RX Dor See W Dor. Cloud non-member?
RY Dor See X Dor.
SW Dor In the region of the Large Magellanic Cloud.
Cloud non-member.
P var [9036].
SX Dor In the region of the Large Magellanic Cloud,
Cloud non-member.
delta(m) var.
SY Dor See W Dor.
According to [9036], variability is doubt-
ful.
SZ Dor In the region of Large Magellanic Cloud,
Cloud non-member.
TT - TW Dor
See W Dor.
TX Dor See X Dor.
TY Dor See SZ Dor.
TZ Dor See X Dor.
UU - UV Dor
See SZ Dor.
UW Dor See W Dor.
UX Dor See SZ Dor.
UZ - VV Dor
The Large
Magellanic Cloud Member?
XX Dor See SZ Dor. [Fe/H] ~ -1.3.
ZZ Dor See SZ Dor.
AA Dor d = 0.02P. Min II 11.21.
alf Dor VB A (B 4.3m, A = 0.2125", P = 13.00yr.)
The
range of combined brightness variations is given.
bet Dor P var. Current elements are given.
T Dra ADS 10937 A (B = UY Dra, optical, 16",
222deg).
U Dra P var. Mean elements are
given.
W Dra P var. Max = 2416748 + 257.11d*E (JD2416750 -
21390); Max = 2430826 + 262.11d*E (JD2421390 -
30820); Max = 2439962 + 268.87d*E (JD2430820 -
40490); since JD2440490 - see
Table.
Y Dra According to visual
observations, 7.8m - 15.0m.
Z Dra Min II 11.0. P var. Min = 2430973.314 + 1.3574176d*E
(JD2428460 - 33300); Min = 2433268.708 +
+ 1.357440d*E (JD2433300 - 43500); since JD
2443500 - see Table.
RR Dra d = 0.015P. Min II 10.1. P var.
Before JD2439000 Min I = 2433390.458 +
+ 2.83123d*E [1001]; since JD2440000 -
see Table.
RS Dra During JD
2436012 - 37584 P = 145.3d.
delta(m)
and the light curve share vary strongly.
RW Dra P var. Mean elements are given.
Composite blazhko effect;
Pi = 93.95P = 41.61d; Pi1 = 280P; Pi2 = 6140P; Pi3 =
= 3400P [1585]. 0.11P <= M - m <= 0.32P. delta(S) = 3.
RX Dra Min II 10.3, d II = 0.009P.
RZ Dra Min II 10.38. P var. Min = 2429448.787 + 0.55087668d*E
(1907 - 1968) [3822]; since 1968 -
see Table.
SU Dra P var. Before 1955 Max hel = 2420605.762 +
+ 0.66041890D; since 1955 - see
Table. [Fe/H] = -1.39.
SW Dra delta(S) = 3.5.
SX Dra d = 0.035P. Min II 10.0. P var. Min I = 2432273.276 +
+ 5.1692d*E (JD2432000 - 38000); since JD
2442000 - see Table.
TT Dra P2 = 198d.
TW Dra ADS 9706 A (B 9.5m vis, 23deg, 3.6"). d = 0.02P; Min II 8.1.
P var. Min I = 2433888.452 + 2.806870d*E (JD
2433000 - 40000) [3825]; since JD2440000 -
Mean elements in the
Table.
TX Dra Mean magnitude var, P2 = 654d.
UU Dra Mean magnitude var, P2 = 960d.
UX Dra According to [9086], the light curve may correspond
to the type E; SB, P ~ 340d.
UZ Dra d = 0.01P; Min II 10.6. Possibly P = 1.65d
[3827].
VW Dra According to photo-
electric observations, 6.28m - 6.32m V.
VX Dra Type E is possible, P = 0.892d/n.
WW Dra Nonlinear term: -4.98d*10**-9*E2.
ADS 10152A (B 9.67m, 8.2", 5deg).
Depth of Min II 0.08m.
WZ Dra delta(m) var strongly.
XY Dra Min II 13.7.
XZ Dra P var. Before JD2438000 Max = 2427985.648 +
+ 0.4764944d*E [0188].
Epochs after JD2438000
are represented dy the elements in the Table only on
average. Blazhko effect; according to [1474], Pi = 78d.
[Fe/H] = -0.57.
ZZ Dra P var. Max = 2434509 + 274.5d*E (JD2416350 -
34600); since JD2437100 - see
Table.
AE Dra delta(S) = (4).
AF Dra VR var; SB?
AG Dra A soft X-ray source. Elements
in the Table represent maxima in U band in 1974 -
1979 [9113].
AI Dra Min II 7.16, D II = 0.17P.
AP Dra Twice shorter pe-
riod is possible.
AQ Dra H beta spectral line is probably filled in by
emission.
AR Dra Min II 11.63.
AS Dra mu = 0.486", P = 289deg. SB. delta(m) var.
Large spatial velocity.
The brightness
varies with the phase of the orbital motion. Phases
of Max and Min vary from cycle to cycle. The Table
gives Porb [3075] and the epoch of the conjunction
(G4 - star is behind).
AW Dra P var. since JD2430500 - see
Table.
AX Dra Min II 11.0.
BE Dra Min II 11.5. The
spectral type is late B.
BH Dra ADS 12019A (B Am, 9.25m, 10.8", 58deg). Min II 8.58.
BK Dra P var.Max = 2415150.817 + 0.592019d*E (JD
2414900 - 16150) [0001]; since JD2416940 -
see Table.
delta(S) = 8 in Max light.
BP Dra Min II 14.7.
BS Dra Min II 9.84.
BV Dra ADS 9537 A (B = BW Dra, 16.3", 358deg, 1980; C 12.69m).
Min II 8.40.
BW Dra ADS 9537 B (A = BV Dra; C 12.69m). Min II 9.02.
BY Dra SB 2 (Porb = 5.9750998d, e = 0.36). mu = 0.365", P = 150deg.
DM var, P var,
(differential rotation),
phase jumps.
Flares up to delta(U) = 1.07m.
CM Dra VB A (B SP = DC, 15.7m pg, 25.7", 22deg, com-
mon mu). mu = 1.619", p = 317deg, pi = 0.068", V nu = -118.6km/s.
Min II 13.63. BY type va-
riability: delta(M) ~<= 0.05mV, P ~ Porb. Flares:
delta(m) ~ 0.05.
CR Dra mu = 0.50", p = 168deg, pi = 0.048".
CX Dra SB, Porb = 6.69612d (with this pe -
riod delta(V) = 0.04m).
Long-term
cyclic variations: P ~ 2400d, delta(V) ~ 0.2m.
Flares ~ 0.1m.
An X-ray source; the reflection effect is
observed.
DE Dra d = 0.017P.
DG Dra Depths respective to Max I
(” = 0.25); Min II 0.17m; Max II 0.01m.
DK Dra Porb = 64.44d.
Epoch of Min is given. Both
components show H and K CaII in emission.
DL Dra VB A (B 9.2m, 3.9", 318deg, 1982). P1 = 0.0825d, A1 =
= 0.028m; P2 = 0.0837d, A2 = 0.026m.
DN Dra P = 109S. mu = 0.32", P = 153deg.
k Dra IR excess.
Fi Dra ADS 11311 (delta(m) = 1.7m, 0.3", 288deg, 1967). A:SB, P =
= 26.768d. The epoch of
Max U light is given.
S Equ Min II 8.11. P var. Before JD2427000 Min =
= 2423746.490 + 3.4360050d*E [1140]; Min =
= 2437968.345 + 3.436072d*E (JD2427000 - 41000)
[3432]; since JD2441000 - see
Table.
Gaseous streams; in Min light H alfa is in emission.
W Equ Min II 12.4. P var.
Z Equ A nearby star: 12.1m.
RT Equ P var strongly.
RW Equ Strong blazhko effect.
RZ Equ Min II 12.2:.
SU Equ Min II 16.4.
SV Equ Depth of Min II 0.16m.
SW Equ Min II 15.6.
NU Equ ADS 14702A (B 11.6m, 2", 268deg; C 12.6m, 48",
optical).
The Table
gives the pEriod of oscillations. Data on the perio -
dicity of the rotational variability of light, spectrum
and magnetic field are contradictory (17.492d, 314d,
1785.7d, 72yr).
V Eri Mean magnitude var, P2 = 1209d.
W Eri SiO, OH, H2O maser.
Z Eri P2 = 746.4d.
RU Eri Min II 9.62.
RX Eri [Fe/H] = - 1.32.
RY Eri d = 0.025P.
RZ Eri d = 0.018P. The depth of Min II 0.04m pg.
SV Eri [Fe/H] = -1.83. P var. P = 0.71365272d (JD2414000 -
21000); P = 0.71370172d (JD2421000 - 26000) [0862];
Max = 2426590.319 + 0.7137406d*E (JD2426000 -
34000) [9195]; since JD2434000 -
see Table.
TT Eri (B - V)Max = +0.255m.
TV Eri (B - V)Max = +0.53m.
TZ Eri d = 0.015P. P var. Min = 2426066.198 + 2.606097d*E (JD
2426000 - 33500) [1490]; since JD2438200 -
see Table.
UX Eri Min II 11.01. P var? Before JD2438500 Min I =
= 2434368.570 + 0.4452820d [2494]; since JD
2438500 - see Table.
UY Eri The shape of the light curve
var. [A/H] = -1.6.
VW Eri Alternating P1 =
83.4d, P2 = 93.3d.
Halo population.
WW Eri Min II 11.2.
WX Eri The depth of Min II 0.22m.
The primary component var,
DSCT:, P1 = 0.16454d, P2 = 0.13721d.
YY Eri Min II 8.72. P var. Min I = 2433617.5198 + 0.321496212d*E
(JD2433000 - 41500) [3850]; since 2441500 -
see Table.
X-ray source.
ZZ Eri Min II 14.4.
AN Eri Min II 14.9.
AO Eri d = 0.04P.
AS Eri Min II 8.42. X-ray source.
BB Eri (k - b)2 = 0.13.
BC Eri Min II 11.26:.
BK Eri delta(S) = 8. P var.
BL Eri The elements
should be checked.
BM Eri P > 20000d; D = 321d; d = 270d.
Only one Min was ob-
served.
Outside Min, according to [5828],
delta(V) = 0.2m, Max = 2440643.0 + 30d*E.
BQ Eri Min II 10.9.
BV Eri Min II 8.42. dII = 0.06P.
BW Eri Min II 9.72.
BY Eri (k - b)2 = 0.06.
BZ Eri Min II 9.21.
CC Eri SB. mu = 0.310", P = 169deg, Pi = 0.083".
Photometric P is close to Porb.
X-ray source.
CI Eri VB (9.9m, 11.2m, 2", 106deg).
CO Eri Min II 9.1.
CS Eri (k - b)2 = 0.03.
CT Eri Min II 10.27.
CW Eri Min II 8.86, DII = 0.10P.
DL Eri P0 - see Table; P1 = 0.118795d [9206]; P2 =
= 0.0968d [9207].
DM Eri ADS 3380 (5.1m, 5.4m, 0.3", 161deg).
Duplicity was obser-
ved only in 1877 and 1923.
DO Eri Epoch of
Min is given. Oscillations with P ~ 6.14 Min, 7 diffe -
rent frequencies have been found. Beat phenomenon,
PB = 12.25d +- 0.47d. Max of the oscillation amplitude
almost coincides with Max of the magnetic field, the
amplitude varies with Prot. Combined amplitude of os -
cillations 0.062m B.
DS Eri Min II 10.3. P var. Min = 2423147.25 + 0.827737d*E
(JD2414869 - 23150); during JD
2423150 - 31320 - see Table.
DW Eri ADS 3409 B (A 6.72m, G8III; B 9", 317deg).
DY Eri ADS 3093 C (A 4.43m V, K1V; B 9.51m V, DA, 82",
105deg; BC A = 7", Porb = 252.1yr). mu = 4.05", P = 212deg.
X-ray source.
DZ Eri Epoch is given for Max (y), Min (He I).
P = 3.67d is possible.
EF Eri 2A0311 - 227. VB A (B 15.8m, 18", 260deg). mu alfa = + 0.147",
mu delta = - 0.070".
Epoch of narrow Min in IR light is gi-
ven. The complex phenomenon of eclipses is descri-
bed in [4041]. Oscillations with P ~ 20.2 and 13.7 Min.
[9211]. Flickering.
EG Eri Epoch of Min in Y
light is given.
EH Eri ADS 3305 A (B 10.8m, 1.45", 60deg, 1917).
gam Eri ADS 2904 A (B 12.4m, 53", 242deg).
lam Eri Shell
features are sometimes present in the spectrum.
nu Eri SB? P2 = 0.1735079d. Beat effect.
omi 1 Eri
P0 - see Table. P1 = 0.1291d.
tau 4 Eri
ADS 2472 A (B 9.9m, 6", 288deg; C 11m, 40", 99deg).
tau 9 Eri
SB 1 (Porb = 5.954d). P = 1.2135d is not
excluded.
S For VB (9.2m, 9.3m, 0.28", 358deg, 1964).
Found unusually bright only on one night
by three experienced observers in europe; harvard pho -
tographs of the same night show it in normal brightness.
V For (B - V)Max = +0.26.
W For Min II is observed.
RX For (k - b)2 = 0.06.
RY For (B - V)Max = +0.535.
SS For (k - b)2 = 0.09.
SW For delta(S) > 10:.
SY For SB 2 [M + pec(eq)].
TZ For SB 2. Possible P values:
37.805d; 44.18d; 50.46d; 75.61d. DI = 1d.
R Gem VB A (B 11.4m pg, 173", 200deg, 1910). S 3.5/6e- S 6.5/6-.
S Gem VB A (B 11.1m, 70", 122deg).
T Gem S 3/4e.
U Gem Min = 2437638.82685 + 0.17690602d*E + 5.4d*10**-12*E**2
[9215]. Depth of Min 0.5m - 1.0m.
Spectrum description [9216].
V Gem P var. Max = 2407750 + 276.2d*E (JD2407700 - 15500);
Max = 2415729 + 278.3d*E (JD2415600 - 21600); Max =
= 2421839 + 269.8d*E (JD2421700 - 26500) [0458]; Max =
= 2432580 + 281.3d*E (JD2427500 - 32600); Max =
= 2434739 + 269.8d*E (JD2432600 - 35800);
since JD2435800 - see Table.
W Gem P var. Max = 2429815.990 + 7.914553d*E (JD2413200 -
31700); since JD2431700 - see
Table. [A/H] = 0.2.
There is possibly faint blue companion.
RR Gem P var. Max = 2415219.734 + 0.39729235d*E (JD
2412000 - 18000); Max = 2418278.900 + 0.39727274d*E
(JD2418000 - 21000); Max = 2422865.229 +
+ 0.39724027d*E (JD2421000 - 25000) [9217]; Max =
= 2427150.267 + 0.3972596d*E (JD2426200 - 27850);
Max = 2434806.289 + 0.3973103d*E (JD2428200 -
34900) [2392]; since JD2436000 -
See Table.
Blazhko effect, PB = 48d [3618],
PB = 37d [9221]. delta(S) = 3.
RW Gem VB A (B 11.04m, 20", 105deg; C 11.84m, 100", 120deg).
Min II 9.74; d = 0.02P.
RX Gem VB A (B 12.65m, 45", 215deg). Min II 9.28; d = 0.004P.
P var. Min I = 2417970.0 + 12.20868d*E (JD2415000 -
27500) [7534]; since JD2427600 -
See Table.
THere is a square term in the ele-
ments given in the Table: +2.25d*10**-7*E**2.
Luminous gaseous ring sur-
rounds the primary component of the system [7535].
RY Gem VB A (B 12.30m, 45", 240deg). Min II 8.75; d = 0.023P.
P var. Min I = 2418015.333 + 9.300876d*E (JD
2418000 - 33000) [8653]; since JD2433000 -
see Table.
Component of A type is surrounded by a
luminous gaseous ring.
RZ Gem VB. P var. Max = 2429632.453 + 5.529716d*E (JD
2415000 - 32400); since JD2432400 -
see Table.
SS Gem 9.9m <= Min II <= 10.7m.
SU Gem P var. Min I = 2429204 + 50.12d*E (JD2429200 - 355)
[0310]; Min I = 2437772.5 + 50.39d*E (JD2437739 -
39850); Min I = 2439856.6 + 50.10d*E (JD2439850 -
40680); since JD2440680 - see
Table.
Mean bright-
ness varies with the elements: Min = 2437953 + 680d*E;
M - m = 264d.
Amplitude of shortperiodical variations is 0.3m - 0.9m.
SW Gem Min brightness epoch is
given.
SX Gem Min II 11.3; d = 0.05P:.
TX Gem Depth of Min II 0.04m; d = 0.017P:.
UV Gem VB A (B 19.5m, 7", 285deg).
WW Gem Min II 10.3.
WY Gem May be an eclipsing system simi-
lar to VV Cep. Atmospheric eclipse began probably
in 1960 - 61, the mean phase of it being in 1968
[5730]. Variable magnetic field [1591, 4498]. Intrin -
sic variability of blue component is also possible
[7536].
YY Gem VB C (A 1.99m, B 2.85m, a = 6.06", P = 306.3 y; C 73",
165deg, 1925); mu alfa = -0.0154s, mu delta = -0.108". Min II 9.59;
Min II - Min I = 0.50P; D = 0.000P. X-ray
source. P const [8655].
Both components are probably UV Cet type
variables. Flare amplitude in the integrated light of
the system reaches 0.3m V, or 1.8m U [9227].
AA Gem [A/H] = 0.0.
AC Gem Min II 11.3. P var. Min I = 2433649.30 + 1.661795d*E
(JD2415000 - 36000) [1530]; since JD
2430100 - see Table.
AF Gem VB A (B 14.8m, 2", 0deg). Min II 10.67.
THere
is a square term in the elements given in the Table:
- 1.71d*10**-10*E**2.
AH Gem Min II 14.8:.
AI Gem Min II 14.0.
AL Gem Min II 9.85.
AN Gem Min II 13.3:; d = 0.037P.
AU Gem OH emission.
AV Gem Min II 12.8:.
AY Gem Min II 10.9.
AZ Gem Min II 12.4.
BB Gem VB A (B 12m, 25", 270deg).
BP Gem P var. Max = 2434120 + 243.9d*E (JD2418700 - 36600);
since JD2436600 - see Table.
BT Gem Min II 14.0:.
CI Gem UG?
CM Gem Min II 15.0.
DL Gem VB A (B 13.1m, 18", 180deg).
DN Gem VB A (B 13.5m, 12", 16deg; C 12.0m, 80", 99deg).
DP Gem Min II 14.0. RRC? P = 0.2792d?
DX Gem P var. Max = 2433182.876 + 3.136226d*E (JD2425000 -
34000); Max = 2435554.199 + 3.136955d*E (JD
2434000 - 36500) [8300]; since JD2436500 -
see Table.
EF Gem P var. Min = 2428108.49 + 6.10222d*E (JD2428500 -
42800) [0407]; since JD2442800 -
see Table.
EL Gem Min II 13.6.
EN Gem Min II 13.8.
EW Gem P var. Max = 2428495.686 + 0.523750d*E (JD2428100 -
30780); since JD2430780 - see
Table.
EY Gem Min II 13.0.
FT Gem Min II 14.1.
GP Gem Min II 13.5.
GR Gem 15.6 <= Min II <= 15.9.
GW Gem Min II 10.68.
GX Gem Min II 11.3.
GZ Gem P = 1.225290d?
HH Gem Min II 13.8.
HR Gem Min II 11.7.
HY Gem Min II 17.5.
II Gem P = 223d?
IP Gem Min II 14.5.
IR Gem In super-
maxima there are superhumps with P = 102 Min [9232].
IZ Gem D >= 0.24d.
KQ Gem Min II 14.6.
KU Gem d = 0.05P.
KV Gem Epoch of Min of brightness is given. EW
type is possible according to the spectrum [9037].
KZ Gem The cycle may be 129d.
LM Gem d = 0.02P.
LX Gem Red.
MO Gem Red.
MP Gem VB.
MU Gem Min II 14.9.
MZ Gem Min II 16.7.
NQ Gem In the spectrum of the carbon
star the hydrogen emission lines and ultraviolet con -
tinuous emission appeared in February 1970 [6348].
NY Gem HD 47396 (Pec) = S 5438 = CSV 798 = CSV 6468.
In the chart in [0156] the position of the va -
riable is wrong.
OS Gem Oscillations with
the period P1 given in the Table are superimposed
by oscillations with the period P0 = 0.070d and smal -
ler amplitude. P1/P0 = 0.78.
zet Gem VB A (B 11.46m, 87", 84deg; C 7.56m, 97", 350deg). P var.
Max = 2410640.42 + 10.15477d*E (JD2394600 -
2407150); Max = 2422366.187 + 10.15288d*E (JD
2407150 - 22300); Max = 2426802.918 + 10.15172d*E
(JD2422300 - 34500) [2392]; since JD
2434500 - see Table.
All the observations are satisfied also by the
elements: Max = 2443785.444 + 10.150135d*E -
5.24d*10**-7*E**2 [9029].
May by a
DCEPS type variable.
eta Gem VB A (B 8.8m, GO III - IV, 1.60", 269.4deg, 1977). SB 1
(P = 2983d [9236]).
Epoch of Min brightness is given. The
deepest minima (corresponding to the middles of the
descending branches of the radial velocity curve) are
satisfied by the elements: Min = 2429355 + 2984d*E
[1551].
mu Gem VB A (B 9.8m, 122", 141deg).
sig Gem VB A (B 10.8m, 182", 316deg); SB 1 (P = 19.603d [9238]).
There is a Min II on the light curve; Min II sometimes
disappears and sometimes becomes deeper then Min I.
Min II - Min I = 0.5P.
U Gru Depth of Min II 0.05m. d = 0.011P.
W Gru P var. Nonlinear term: +7.84d*10**-9*E**2. Min II 10.0.
X Gru d = 0.008P. Min II 10.69. P var.
Current elements are given.
Z Gru delta(S) = 12:.
The shape of the light curve and P are strongly
variable.
RS Gru (k - b)2 = 0.22.
RT Gru (k - b)2 = 0.02. Blazhko effect.
RV Gru (B - V)Max = +0.93. Min II 11.4.
RW Gru delta(S) = 10. Blazhko effect.
RX Gru Min II 10.7.
RY Gru Superposition
of irregular variations?
During JD2434513 - 517
Precalculated
minima were not observed.
RZ Gru A description
of light changes [2809].
UW Gru [Fe/H] = -1.6.
VW Gru P >= 260d?
VY Gru P > 160d.
VZ Gru RR type is also possible.
AK Gru Elements
should be checked.
AP Gru P var. Mean elements JD
2427992 - 36848 - see Table.
during JD2434250 - 36848 Max = 2434337.337 +
+ 0.5082945d*E.
AR Gru Min II 10.6.
AV Gru P >= 160d is possible.
AW Gru Min II? JD2436818.
BC Gru Min II 10.3. RRC type is pos-
sible.
BD Gru Min II 14.9.
BH Gru Min II 15.2:.
pi 1 Gru
VB A (B 10.9m, G0V, 2.7", 202deg).
T Her VB A (B 10m, 67", 321deg).
U Her SiO, OH, H2O maser.
W Her ADS 10121 A (B 14.2m, 6", 334deg).
X Her P2 = 746d.
Z Her VB A (B ro > 10"). Min II 8.18.
nonlinear term: -6.19d*10**-10*E**2.
RU Her SiO maser.
The spectrum in Min
light is composite; a companion? [3502].
RX Her Min II 7.74.
SW Her B - V; +0.12, +0.40. P var. Before 1921 Max =
= 2416687.018 + 0.4928864d*E.
SX Her [Fe/H] = -1.8.
SY Her On period varia-
tions see [8699].
SZ Her Min II 10.10. P var. Min = 2430766.8390 + 0.818096d*E +
+ 0.0165d sin (0.010465deg*E + 180deg) [5749].
The Table gives current elements satisfac -
tory after JD2438000.
TT Her Min II 9.89. The light curve
shape var.
P var. Before JD2430000 Min = 2425433.627 +
+ 0.9120846D [2389]; Min = 2434525.2572 + 0.9120800d*E
(JD2430000 - 40000) [3504]; since JD
2440000 - see Table.
TU Her d = 0.022P. P var. Before JD2435000 Min =
= 2424381.416 + 2.2671303d*E - 854d*10**-11*E**2 [9240];
Min = 2437462.3909 + 2.2669718d*E (JD2435000 -
38000) [9241]; Min = 2443324.70097 + 2.2669385d*E
(JD2438000 - 44000) [8593]; since JD
2444000 - see Table.
TW Her [Fe/H] = -0.47.
TX Her Min II 8.97, DII = 0.11P. P var;
periodic term: +0.0081d sin [0.042deg (E + 7255)].
UU Her [Fe/H] = -1.27.
There was alternation of periods 90d and 71d
[0310]; the period 45d [3507] was also noted.
During JD2443611 - 44161 -
see Table.
Epoch of Min is given.
UX Her Min II 9.11. P var. Before JD2429000 Min =
= 2419876.467 + 1.5488598d*E [0279]; Min =
= 2429987.420 + 1.5488513d*E (JD2429000 - 38000)
[3671]; since JD2438000 - see
Table.
VW Her VB A (B 17.3m, 18", 120deg.
VX Her delta(S) = 5. P var; nonlinear term:
- 0.00745d (E:10000)**2.
According to [3369],
a member of an eclipsing binary system.
VZ Her [Fe/H] = -0.9. P var. P = 0.44031880d (JD2415000 -
22000) [5738]; Max = 2425004.4590 + 0.44032394d*E
(JD2422000 - 27000); Max = 2425004.4456 +
+ 0.44032631d*E (JD2427000 - 36000) [3506];
since JD2436000 - see Table.
WW Her VB A (B 15.6m, 7.4", 148.5deg, white).
WX Her Twice longer P is
not excluded.
AC Her P var.
The
Table gives current elements valid since JD
2442000. Mean P = 75.4619d [1754]. The magnitude in
Max varies with delta(m) = 1.6m [0368].
AD Her VB A (B 11.97m, 5", 189deg). d = 0.033P. Min II 9.79.
AF Her P var. Before JD2426950 P = 0.630336d;
since JD2426950 - see Table.
The shape of the light curve
var.
AG Her P var. Max = 2422935.584 + 0.6494378d*E (JD
2418210 - 26952); since JD2426952 -
See Table.
AH Her Porb = 5.9d:. Oscilla-
tions during outbursts: 24s <= P <= 39s, delta(m) <= 0.003m [9251].
Flicckering in Max And Min up to 0.4m in 2 -
8 minutes [9252].
AK Her ADS 10408 A (B 12.0m, 5", 323deg). Min II 8.64. Min II -
- Min I = 0.505P. dII = 0.07P. P var. Before JD
2421200 Min = 2421200.549 + 0.42152207d*E; Min =
= 2421200.549 + 0.42152083d*E (JD2421200 - 24950);
Min = 2424949.555 + 0.42152061d*E (JD2424950 -
30000) [1760]; Min = 2430939.368 + 0.42152362d*E
(JD2430000 - 41500); since 2441500 -
see Table.
The shape of the light curve
var.
AM Her ‡U 1809 + 50. Lx(soft)/Lopt ~ 15.
Emissions of H And
KCaII, H, HeI, HeII, etc. In the spectrum. Epoch of
Min I in V light is given. The period shows complex
variations. The phase of Min I in U light is 0.30p, in
B 0.15P, in R 0.05P. Min I is probably due to an ec -
lipse of a hot spot and the gas flow near the surface
of the white dwarf by the white dwarf itself. The
depth of Min I is up to 0.7m. Min II with the depth up
to 0.4m (sometimes absent), Min II - Min I = 0.55P. Min II
coincides in phase with the X-ray eclipse. High and
low states (b ~ 13.0m and B ~ 15.0m on average); in
the high state there are variations with delta(m) ~ 0.3m on
the time scale >= 200d; the duration of low states is
130d - 700d [9258] or less. During low states the
depth of minima is small. Flickering up to 0.8mV in
several minutes or dozens of seconds; X-ray flicke -
ring on the time scale of ~ 10s not correlating with
optical flickering. The magnetic field ~ 1*10**7 G at
the equator, ~ 2*10**7 G on poles. Variable circular
(from +3% to -9%) and linear (up to 7%) polarization.
IR excess at lambda 10 mkm.
AP Her P var strongly. P = 10.400d (JD2415000 -
19000:); P = 10.3970d (JD2423700 - 24700:); P =
= 10.4260d (JD2424700 - 25300); P = 10.4338D (JD
2425800 - 27000); P = 10.3945d (JD2427000 - 27400);
P = 10.4277d (JD2433000 - 33850); P = 10.3898d (JD
2433850 - 34850); P = 10.4209d (JD2434850 - 35600);
P = 10.3715d (JD2435600 - 37200);
DURING JD2437200 - 43800 - see Table.
The light curve shape var.
[A/H] = -0.8.
AR Her P var in a complicated way. Max =
= 2424794.274 + 0.4700234d*E (1905 - 1954) [6535];
Max = 2439692.683 + 0.469975d*E (1954 - 1967) [5274];
since 1967 - see Table.
Blazhko effect, Pi = 31.5489d [3555],
delta(m) var (0.9m -: 1.8m pg) [2168], (M - m) var. delta(S) = 6.
AT Her The star is bright on one
plate (JD2418209).
Besides that, 11.8m - 12.25m.
AW Her VB A (B 10" - 20"). d = 0.03P.
BB Her P var. P = 7.507696D (JD2418924 - 30700);
since JD2430700 - see Table. [A/H] =
= +0.3.
BC Her P var. Before JD2432000 Min = 2426242.372 +
+ 3.08752d*E [9262]; since JD2436000 -
see Table.
BD Her P var. P = 0.4739135d (JD2426540 - 29620); P =
= 0.4739057d (JD2429620 - 30570); Max = 2430495.404 +
+ 0.4739126d*E (JD2430570 - before 1948) [9263];
since 1948 - see Table. delta(S) = 0.8.
BL Her P var. P = 1.3074604d (JD2415000 - 35000);
since JD2435000 - see Table.
Another possible
representation: Max = 2434999.402 + 1.307457d*E
- 3.9d*10**-10*E**2 (JD2415000 - 42000). [Fe/H] = 0.0.
BO Her d = 0.015P. Min II 10.8. P var?
CC Her P var. Min = 2426120.415 + 1.7340314d*E (JD
2425790 - 31265); Min = 2431265.288 + 1.7340460d*E
(JD2431265 - 36000) [2389]; Min = 2439668.342 +
+ 1.73398d*E (JD2436000 - 39600); since JD
2439600 - see Table.
CD Her The chart in [6286] is
wrong.
CE Her [A/H] = -1.8.
CK Her P var? Max = 2429231.234 + 0.519201d*E (JD2429231 -
877) [0332]; during JD2436041 -
37955 - see Table.
CO Her P2 = 600d. So-
metimes does not vary for 150d.
CP Her Superimposed waves, 50d -
100D.
CT Her The depth of min II 0.05m. P var.
Min = 2430904.431 + 1.786337d*E (JD2426480 - 35000)
[3567]; Min = 2439355.666 + 1.7863645d*E (JD
2435000 - 39500) [0001]; Min = JD2441499.3307 +
+ 1.7863891d*E (JD2439500 - 42500) [8593];
since JD2442500 - see Table.
DE Her P var. Max = 2425754 + 171.2d*E (JD2425754 - 30890);
Max = 2430889 + 175.3d*E (JD2430890 - 36150);
during JD2436150 - 38140 - see
Table.
DF Her Elements are valid
since JD2425900.
DH Her d = 0.024P:. Min II 9.5.
DI Her Min II 8.95, DII = 0.03P, Min II - Min I = 0.77P (1966 -
1978). Apsidal motion: P =
= 29000yr +- 4000yr; Min II = 2442241.4602 +
+ 10.5501751d*E.
A considerable discrepancy between the observed and
the theoretical rate of apsidal motion.
DK Her P var.
DL Her Blazhko effect, Pi = 33.6d, 11.0m <=
<= m Max <= 11.3m. P var. delta(S) = 5.
DO Her Close to V362 Her.
DQ Her VB A (B 18.17m, F, 3.5", 132deg, optical?).
Nebula, R = 10.5" (H alfa, 1981).
After the main Max of the Nova a deep
Min 13.0m (JD2426925) and a flat secondary Max
6.7m (JD2427065) were observed.
Eclipsing variability:
14.61m - 18.08m, Min HeI = 2434954.9445 + 0.193620877d*E
[9280]. D = 0.20P, d = 0.000P.
The light curve shape
and delta(M) var.
Oscillations: Max HeI = JED
2434954.785868 + 8.22521640d*10**-4*E - 2.8048d*10**-16*E**2
[8722], 0 <= delta(m) <= 0.08m.
Polarization changes with double oscil-
ation period.
Flickering: delta(m) = 0.15m.
DY Her P var, nonlinear term: -18.6d*
*10**-13*E**2.
EI Her Red.
EN Her P var. Before JD2427000 P = 160d.
ES Her Min II 13.7.
ET Her The ele-
ments are valid earlier than JD2427200
EX Her Red.
EZ Her The ele-
ments are valid earlier than JD2427400.
FN Her P var?
FW Her Min II 14.6.
FY Her According to the
spectrum, EW type is possible.
GL Her P var?
GU Her d = 0.010P. Min II 11.8. Min II - Min I = 0.513P.
GV Her [Fe/H] = -1.41. P var. Max = 2427543.360 +
+ 0.2914606d*E (JD2427543 - 29728) [0152];
during JD2436041 - 38170 - see
Table.
GY Her P var. Max = 2428219.623 + 0.524347d*E (JD2428219 -
727) [0152]; during JD2436370 -
38170 - see Table.
HS Her d = 0.025P. Min II 8.63. P var; since JD
2438240 - see Table.
Apsidal motion: Pi ~ 130yr
[6538].
HV Her d = 0.008P:; Min II 12.9:.
HZ Her Her X-1 = 4U 1656 + 35. Lx/Lopt = 2 - 60.
The Table gives elements for light minima due
to eclipsing variability and the reflection effect. Min I
coincides with the X-ray eclipse. Shallow Min II may
be present. The reflection effect causes variations
with delta(m) up to 1.5m. A cycle of 34.875d duration is
observed in X-ray band; the source is faint during
two thirds of the cycle. The optical light curve chan-
ges are observed during the 35d cycle [9283]. Ac-
cording to [6539], during JD2427543 - 657 and JD
2428630 - 29789 the strong reflection effect was ab-
sent; the star was still varying with P = 1.7d and had
delta(m) ~ 0.5m, Min I = Min II. In [6546] it is stated that
such intervals with no reflection effect, of 8d to 7a
duration, took place for almost half the time since
1890. The light changes during such intervals are in
the range 14.7m - 15.2m pg. Since 1957 intervals wit -
hout the reflection effect were not observed. In June -
July 1983 the predicted phases of high X-ray flux
did not take place, but the reflection effect did not
disappear [9284]. Secondary light variations: P1 =
= 1.0977d (delta(B1) = 0.33m), P2 = 0.871173d*E (delta(B2) = 0.10m),
P3 = 1.623846d*E (delta(B3) = 0.17m) [9285]. X-ray pulsar,
P = 1.2377991s (JD2443357), dP/dt/P = (-2.9 +- 0.2)*10**-6/yr
[9286], sometimes noticeable also in the
optical range [6543]. Rapid brightness flickering.
IK Her d = 0.030P?
IQ Her Superposition of variations with shorter P and
small delta(m) [6645].
IT Her See FY Her.
KL Her Min II 14.7.
KV Her The light curve is characteristic of Mira Ceti stars
but strongly varies. Many irregularities. O - C: -96d,
+73d.
LR Her Min II 15.4:.
LS Her The light curve shape var.
LT Her d = 0.02P. Min II 10.79.
LV Her P var? During JD2428429 - 31342 -
see Table.
MM Her VB A (B 13.50m, 18", 120deg). Min II 9.7.
delta(m) of the distorsion wave up to
0.12m.
MP Her [Fe/H] = -1.18.
MS Her Min II 13.3.
MT Her Min II 12.30.
MV Her The chart in [0156] iden-
tifies the variable erroneously; real MV Her is mar -
ked as "C".
MW Her P var. P = 503d (1976) [9290]. During
JD24668 - 29172 - see Table.
MX Her Moments of Min after
JD2444000 published by different groups of obser-
vers contradict each other.
NQ Her According to [3882], EA, 8.0 - 8.6 pg, Min II
8.4, Min I = 2426894.433 + 0.870218d*E (JD2426894 -
34250).
NR Her Waves, P = 2.8d - 5.5d.
OQ Her Epoch of min is given.
OS Her B - V: +0.12, +0.48.
OU Her Spectral
type is given according to [2198]; in BSD-G7.
OX Her delta(S) = 6:.
PW Her Min II 10.1; DII ~ 0.3P( ).
V338 Her Min II 10.13. P var. Before JD2437000 Min =
2433771.38 + 1.305732d*E [3115]; Min = 2441864.379 +
+ 1.3057515d*E (JD2437000 - 43400) [8593, 0001];
since JD2443400 - see Table.
V342 Her Min II 10.7.
V347 Her P var. Max = 2415288.21 + 0.5373619d*E (JD2415288 -
18596); since JD2429495 - see
Table.
V359 Her P var. Min = 2416046.476 + 1.755754d*E (JD2416000 -
26500) [0001]; Min = 2435693.47 + 1.755775d*E (JD
2426500 - 36000) [1040]; since JD2443500 -
see Table.
V362 Her Close to DO Her.
V365 Her Blazhko effect: Pi = 40.64d. P var.
During JD2429037 - 36840 -
See Table.
V373 Her P = 0.33d or 0.50d is possible.
V384 Her See V373 Her.
V387 Her Min II 13.2.
V394 Her P var?
V395 Her Z = 0.0643.
V396 Her Z = 0.175.
V403 Her Min II 16.0:.
V412 Her Min II 15.2.
V422 Her P var? During JD2434131 - 35991 -
see Table.
V423 Her Min II 15.0.
V426 Her Min II 15.8.
V431 Her P var.
V436 Her The elements are uncer-
tain.
V441 Her IR excess,
evidence for a circumstellar envelope. Possibly non -
radial pulsation.
V442 Her P var. Max = 2434223.375 + 0.4421143d*E (JD
2417447 - 36083); since JD2435730 -
see Table.
The shape of the
light curve varies.
V446 Her Before the outburst 16.2m - 18.8m [3607].
V451 Her ADS 10310 A (B 10.70m, 19", 239deg).
The epoch of Min U light is given.
V458 Her [Fe/H] = -1.65.
V463 Her P = 54.4d is possible.
V477 Her Min II 15.4.
V482 Her Possibly eclipsing.
V499 Her Blazhko effect.
V502 Her Min II 13.5?
V510 Her P var?
V511 Her P var?
V513 Her Min II 15.7.
V516 Her Min II 17.1.
V523 Her Elements are va-
lid during JD2430940 - 990.
V524 Her Twice shorter P is
possible.
V527 Her Max = 2430938.451 + 0.5188d*E (JD2430938 - 990);
during JD2436308 - 318 - see
Table.
V529 Her Epoch of Min is given.
According to [4217], P = 120d.
V533 Her VB A (B 16m, 9.5", 0deg). oscillations:
Max = 2443717.730281 + 0.0007364941d*E, A ~ 1%
[4162].
V551 Her P = 4.00d/n is possible.
V552 Her P = 3.04d/n is possible.
V554 Her P = 4.01d/n is possible.
V557 Her P = 8.00d/n is possible.
V570 Her P = 0.5d or 0.33d is possible.
V578 Her Red.
V582 Her VB. Red.
V583 Her Red.
V588 Her Possibly eclipsing.
V600 Her SB, Porb - see Table.
Variability of Vr possibly cau-
sed by BCEP type pulsations: P - 0.18d.
V601 Her Ele-
ments are valid since JD2439184.
V604 Her Red.
V608 Her Blazhko effect.
V615 Her Red.
V618 Her P var?
V624 Her VB A (12.04m, 40"). Min II 6.35. SB 2.
V637 Her ADS 10227 A (BC 9.2m, 9.2m, 1.7", 18deg, 1975; BC: A =
= 0.28", Porb = 56.56yr).
V639 Her mu alfa = - 0.21", mu delta = + 0.39",pi = 0.087". VB B (A = V647 Her,
11.36m var, dM4e; B 16", 268deg).
Flares in the bAnds U And M pg.
V640 Her VB A (B 14.9m, 8.5", 217deg; C 13.9m, 23", 221deg).
V641 Her L or ISB type is
also possible.
V644 Her SB (Porb = 11.859d).
V645 Her P ~ 3h - 10h, a cycle of 40d.
V647 Her VB A (B = V639 Her, 16", 268deg); mu alfa = -0.21", mu delta =
= +0.39"; pi = 0.087".
V652 Her P var; nonlinear term: - 45.80d*
*10**-10*E**2. delta(m) var.
Resembles PV TEL type
stars but is a helium rich subdwarf. Epoch of Max is
given. Secondary hump at the phase 0.5P.
V654 Her delta(m) = 0.15m in white light.
V655 Her ADS 10407 A (B 9.2m, 4.1", 144deg, 1971).
V657 Her According to [2610], CST?, 11.0m.
V662 Her Less probable P va-
lues: 0.56629d, 0.56710d, 0.56881d, 0.56970d.
V685 Her Min II 15.8.
V687 Her Min II 14.9.
V691 Her Possible P values: 0.927d,
0.637d.
V697 Her H2O, OH maser.
V699 Her Min II 16.0:.
V717 Her Blazhko effect?
V718 Her Min II 14.3.
V719 Her EW type with twice longer P is not excluded.
V720 - V721 Her
See V717 Her.
V722 Her Min II 15.7.
V723 Her Min II 15.5.
V728 Her Min II 11.4.
V731 Her Min II 13.8.
Twice shorter P is not excluded.
V732 Her Min II 13.8.
V733 Her Min II 14.3:.
V737 Her See V717 Her.
V740 Her Min II 14.4.
V741 Her See V717 Her.
V742 Her Min II 14.4.
V744 Her Vr var, P = 86.7221d (SB1?
nonradial pulsatiob?).
Rapid spectral variability is possible: P = 2.5552d,
0.78906d.
V749 Her P = 465s.
V771 Her Epoch of max U light
is given.
V772 Her VB AB (7.4m, G0V; 8.5m, G8V:; A = 0.27", E = 0.97, P =
= 20.0yr, C 10.62m, 28").
One of the components
(probably B) is SB1, P = 0.879511d [4056]. The same
component must be the eclipsing system. Faint X-ray
source.
V774 Her Both flares and "antiflares" (abrupt fadings) of com-
parable amplitude are observed.
alf Her ADS 10418 A (B 5.39m, 4.9", 107deg, 1973; B - SB2, G5III +
+ F2V).
Slow variations, P ~ 6yr, delta(m) ~ 0.5m; quicker changes,
P ~ 50d - 155d, delta(m) ~ 0.3m - 1.0m.
TogetHer with the visual companion the
star is surrounded by an enormous envelope (R ~ 2*10**5R$,
expansion velocity 10 km/s, mass loss 3*10** ~ 8M$/YR).
nu Her [Fe/H] = - 0.26. SB?
omi Her VB interferometric.
ome Her ADS 10054 A (B 11.5m, 0.8", 232deg, 1967; C 11.0m, 28.4",
96deg, 1957; D 27.5", 271deg, 1960).
Epoch of Min is given. Double wave
in the light curve. Rapid variations, P = 0.15d [9310].
g Her The mean cycle 1972 - 1981 is given. SLow
pulsations ( = 875d +- 70d) and non-periodic varia-
tions on the time scale of 5d - 15d with delta(m) up to
0.2m are superimposed.
u Her ADS 10449 A (B 10.2m, 4.4", 60deg). Min II 4.93.
R Hor OH, H2O, SiO maser. P var. Max = 2428868 +
+ 401.5d*E (JD2412800 - 28900); since JD
2428900 - see Table.
V Hor
= 59d (JD2428380 - 910),
= 90d (JD
2429170 - 980).
X Hor Epoch of
Min brightness is given. Maxima are broad. Usually
secondary minima are observed.
SY Hor Min II 12.0.
SZ Hor Min II 10.7:.
TU Hor Min II 6.03; Min II - Min I = 0.52P;
Max II is fainter than Max I by 0.05m. Pe -
culiar ellipsoidal variable [9245].
TY Hor Type RCB?
UU Hor P var. Max = 2416826.417 + 0.6436900d*E (JD
2416800 - 25000); since JD2425000 -
See Table.
UX Hor Min II 14.4. P var. Min I = 2426659.380 + 0.7126943d*E
(JD2426650 - 30860); since JD2430540 -
see Table.
UZ Hor P var. Max = 2426679.425 + 0.338188d*E (JD2426300 -
28430); since JD2430040 - see
Table.
VY Hor mu = 0.173", ro = 33deg. P = 314s, 617s.
R Hya VB A (B 13.0m, 21.6", 324deg). SiO maser.
P var. According to [0458]; Max =
= 2328201 + 486d*E (JD2328200 - 31120); Max =
= 2343512 + 507d*E (JD2343300 - 44800); Max =
= 2372678 + 485d*E (JD2372200 - 72700); Max =
= 2380447 + 477d*E (JD2380000 - 81400); Max =
= 2385160 + 461d*E (JD2384700 - 88000); Max =
= 2394350 + 448.6d*E (JD2393900 - 2402000); Max =
= 2403742 + 434d*E (JD2403300 - 04200); Max =
= 2406363 + 429.5d*E (JD2406000 - 11100); Max =
= 2413642 + 411d*E (JD2413200 - 14100); Max =
= 2416563 + 405.5d*E (JD2416100 - 23400); Max =
= 2424288 + 414.7d*E (JD2423400 - 28500).
since JD2428500 - see Table.
T Hya P var. Max = 2399455 + 289.00d*E(JD2398600 -
2421700); Max = 2422584 + 294.2d*E (JD2421700 -
25800); Max = 2431781 + 284.20d*E (JD2425800 -
36200); since JD2437500 - see
Table.
V Hya VB A (B 11.58mV, KO III, 46", 186deg).
Mean brightness varia-
tions with P = 6670d and A = 3.5m are superimposed
by light oscillations with A = 1.1m - 2m and elements
given in the Table. Deep light minima were obser -
ved in 1891, 1908, 1925, 1942 - 43, 1959, and 1962.
A graph of the light curve [3614].
W Hya VB A (B 9.3m, 72", 108deg). P var. Max = 2411074 +
+ 379d*E (JD2411000 - 14150); Max = 2414644 +
+ 395d*E (JD2414150 - 19400); Max = 2419746 +
+ 378d*E (JD2419400 - 25200) [0458]. Max =
= 2425740 + 366d*E (JD2425200 - 27000); Max =
= 2440336 + 397.35d*E (JD2428000 - 40500);
since JD2440500 - see Table.
Amplitude and shape of the light curve vary
strongly.
OH, H2O, SiO maser.
X Hya OH, H2O, SiO maser.
Y Hya Mean magnitude va-
ries.
RR Hya H2O maser.
RS Hya P var. Max = 2422973 + 330.2d*E (JD2414000 - 23000);
Max = 2429126 + 342.0d*E (JD2423000 - 29200); Max =
= 2429455 + 331.2d*E (JD2429200 - 34500);
since JD2434500 - see Table.
RT Hya Before 1952
= 255d; since 1952 -
see Table.
The character And amplitude of light varia -
tions vary strongly.
RU Hya OH, H2O maser. P var. Max = 2429572 +
+ 334.0d*E (JD2414000 - 29600); since JD
2428500 - see Table.
RW Hya SB 2 (P = 370d). Epoch
of Min brightness is given.
RX Hya VB A (B 10.5m). Depth of Min II 0.05m. P var.
Min I = 2428261.385 + 2.2815942d*E (JD2419500 -
28500); Min I = 2440650.409 + 2.2816200d*E (JD
2428500 - 41400); since JD2441400 -
see Table.
SS Hya VB A (B 12.0m, 13", 195deg); SB 2.
SU Hya Mean mag-
nitude varies with P = 780d.
SV Hya VB A (B 35", 225deg). delta(S) = 7.
SX Hya D = 0.022P. P var. Min I = 2427659.223 + 2.895697d*E
(JD2410000 - 28000) [0007]; since JD
2442500 - see Table.
SY Hya P var. Min = 2425590.589 + 3.403082d*E (JD2425500 -
31150) [7548]. Since JD2432200 -
See Table.
SZ Hya P var. Max = 2415714.1429 + 0.53742815d*E (JD
2414700 - 26500) [3626]; Max = 2426410.575 + 0.53736d*E
(JD2426400 - 27200) [0001]; Max = 2431881.5537 +
+ 0.53723051d*E (JD2427880 - 35200) [3626]; Max =
= 2435542.267 + 0.5372497d*E (JD2435500 - 38900)
[3627]. Since JD2438770 - see
Table.
Blazhko effect: Max(A) = 2440705 +
+ 25.8d*n [6557]; 10.44m <= Max <= 11.03m.
TT Hya Min II 7.32; d = 0.035P.
TU Hya P var. Max = 2416980 + 277.5d*E (JD2412500 -
17300); Max = 2417260 + 272.5d*E (JD2417200 -
19800) [1787]; Max = 2430410 + 281.4d*E (JD
2420500 - 30500); Max = 2438332 + 272.3d*E (JD
2432000 - 39200); since JD2439200 -
see Table.
TY Hya P var. Min = 2434478.464 + 4.660978d*E (JD2419800 -
35000) [1788]; since JD2435000 -
see Table.
UU Hya P var. Max = 2427423.84 + 0.5238585d*E (JD2414950 -
27400) [1789]; Max = 2429729.835 + 0.523854d*E (JD
2427000 - 31000) [0752]. Spectrum
is based on Ca II.
UW Hya Min II 13.8:; Min II - Min I = 0.64P. P = 1.055439d?
UY Hya Min II 13.8. RRC?
VV Hya P var. Max = 2427421 + 155d*E (JD2419500 - 37000)
[1792]; since JD2437000 - see
Table.
VX Hya (k - b)2 = 0.26.
Luminosity class
[3149] contradicts the type of light variability. The
shape of the light curve strongly varies. The main
oscillation with the period P0 given in the Table is
superimposed by the secondary one with P1 = 0.172720d
[3631]. P1/P0 = 0.773; Pb = 0.761445d.
VY Hya Min II 9.1.
VZ Hya Min II 9.46.
WY Hya Min II 11.2.
WZ Hya (k - b)2 = 0.06. P var. Max = 2416169.681 + 0.53772640d*E
(JD2414000 - 19000); Max = 2419811.736 +
+ 0.53775858d*E (JD2419000 - 21000); Max =
= 2424618.630 + 0.53774101d*E (JD2421000 - 32000)
[0752]; Max = 2436613.445 + 0.5377229d*E (JD
2436600 - 38500) [3633]; since JD2438000 -
see Table.
XX Hya P var. Max = 2439560.355 + 0.50774868d*E (JD
2428200 - 39560) [5238]; since JD2439560 -
see Table.
XZ Hya Min II 15.0.
AE Hya Min II 14.6.
AF Hya Min II 13.8.
AI Hya Min II 9.84; Min II - Min I = 0.438P; DII = 0.075P; dI = 0.02P;
dII = 0.00P; EA/DM. Pulsation
period P' = 0.13803d, A = 0.02m - 0.03m [9259].
AV Hya Min II 10.35; dI = 0.023P:.
CH Hya Min II 15.5; Min II - Min I = 0.57P.
CW Hya P var? [4027].
Elements given in the Table
satisfy observations only in the interval JD
2428950 - 30375.
DD Hya P var. Max = 2431139.313 + 0.501818d*E (JD2431100 -
600) [1432]. Since JD2441600 -
see Table.
DE Hya d = 0.014P?
DF Hya Min II 11.5.
DH Hya delta(S) = 7.
DK Hya Min II 10.7.
DM Hya d = 0.15P?
EU Hya Min II 10.2.
EX Hya Light variations with Porb and amplitude up to 0.9mV
due to eclipses of hot spot are represented by the
elements: ET(Min) = 2437699.94177 + 0.0682338422d*E,
where ET(Min) is the heliocentric Julian Date con -
verted to Ephemeris Time; simultaneously periodic
modulation of the shape of the light curve between
the outbursts is observed with the amplitude 0.2m -
0.9m and the elements: Max = 2437699.8895 +
+ 0.04654656d*E - 1.2d*10**-12*E**2 [9265]. Mean inter-
val between bright outbursts is 465d [5695], mean
cycle is close to 20 - 30d.
EY Hya P var. Max = 2432707 + 160.5d*E (JD2426100 - 32800);
since JD2432800 - see Table.
EZ Hya Min II 10.7. P var. Min I = 2440255.8482 +
+ 0.44976658d*E (JD2431160 - 40650) [7549];
since JD2440250 - see Table.
FG Hya Min II 10.25; dI = dII = 0.085P. P var. Min I =
= 2431150.388 + 0.3278422d*E (JD2431140 - 34400)
[0182]; Min I = 2436968.7067 + 0.32783433d*E (JD
2434050 - 400) [3639]; Min I = 2436968.7067 +
+ 0.32783546d*E (JD2436950 - 43250) [9267];
since JD2444600 - see Table.
FI Hya V27 in the globular cluster NGC 4590
(M68); cluster non-member.
FS Hya According to [1480] P = 91.7d.
FW Hya Min II 12.4.
FY Hya VB A (B 15.45m, 15", 90deg); delta(S) = 7:; (k - b)2 = -0.03.
GK Hya Min II 9.57.
THere is a square term in the elements:
- 4.01d*10**- 9*E**2.
GM Hya d <= 0.01P.
GN Hya Min II 13.6.
GT Hya Cep?
HS Hya Min II 8.55.
IK Hya Blazhko effect with Pi ~
= 30d.
IW Hya OH, H2O maser.
KM Hya P var?
KU Hya VB AB (7.3m, 7.4m, A = 0.150", P = 58.93 yr, E = 0.219);
A(v) = 0.06m.
KW Hya Porb = 7.75043d; E = 0.110 [9273]; Min II 6.35; Min II -
- Min I = 0.54P.
bet Hya VB A (B 5.6m, 0.9", 8deg, 1959).
khi 2 Hya Min II 5.92.
R Hyi The member of
the Small Magellanic Cloud.
Y Hyi d = 0.024P.
RS Hyi In the region of the Small Magellanic Cloud.
Not a member of the cloud.
RT Hyi Min II 14.1.
RV Hyi Min II 12.4; Min II - Min I = 0.61P.
RY Hyi See RS Hyi.
RZ Hyi See R Hyi.
ST Hyi See R Hyi. [A/H] = - 0.8.
SZ Hyi See RS Hyi.
TW Hyi delta(S) = 10:.
UU Hyi P = 112.25d?
VW Hyi Mean interval between the
supermaxima is 179d. Porb = 0.0742711d. Between the
normal outbursts the brightness periodically increa -
ses by 0.35m - 0.40m because of hot spot appearances:
Max = 2440128.0222 + 0.0742711d*E [7550]. During the
supermaxima the period between the superhumps is
0.0769d [9275]. Sometimes the light oscillations with
the amplitude 2% and cycle from 28s to 34s are ob-
served [7551].
VY Hyi See RS Hyi.
VZ Hyi RR [0193].
WX Hyi Mean interval between the super-
maxima is 141.5d. Porb = 0.0748134d [9277]. Period
between the superhumps observed during the super-
maxima is 0.07737d [9278].
WZ Hyi See RS Hyi.
XY Hyi See R Hyi.
AC Hyi See RS Hyi.
AH Hyi See R Hyi.
AI Hyi See R Hyi.
BB Hyi delta(S) = 7:.
V Ind P var. Max = 2439792.276 + 0.4796030d*E (JD
2414000 - 40000) [5233]; since JD2440000 -
see Table.
delta(S) = 7, (k - b)2 = 0.02.
RS Ind Min II 10.0. P var.
RU Ind VB A (B 12.6m, 2.3", 103deg). Min II 12.1.
RX Ind 240d < P < 310d.
RY Ind Min II 11.04.
ST Ind Min II 11.79.
SU Ind Min II 9.5:.
TV Ind Min II 11.9.
AR Ind Min II 14.4. RRC?
AY Ind mu alfa = +0.345", mu delta = -0.310"; VB?
R Lac VB A (B 14.1m, 6", 50deg).
S Lac P var. Max = 2412857 + 238.2d*E (JD2410000 - 16400);
Max = 2418828 + 241.45d*E (JD2416400 - 20500); Max =
= 2427307 + 242.7d*E (JD2420500 - 27300); Max =
= 2437290 + 237.4d*E (JD2427300 - 37300);
since JD2437300 - see Table.
U Lac There
are light variations with the periods: 150d, 550 - 690d,
2900d.
V Lac P var. There
is a square term in the elements: - 6.48d*10**-8*E**2.
W Lac P var. Max = 2415255 + 323d*E (JD2414600 - 15300);
Max = 2425628 + 335.5d*E (JD2425600 - 38000) [0458];
Max = 2433844 + 324.5d*E (JD2428000 - 33850);
since JD2433850 - see Table.
X Lac P var. Max = 2418890.497 + 5.444303d*E (JD2416670 -
29500) [2033]; since JD2429500 -
see Table.
Z Lac P var.
There is a square term in the elements: -3.4d*10**-8*E**2.
[A/H] = 0.2.
RR Lac P var. Max = 2419434.331 + 6.416146d*E (JD2417900 -
31600); since JD2431600 - see
Table. [A/H] = 0.0.
RT Lac Min II 9.62. P var. Min I = 2440382.9005 + 5.0740484d*E +
+ 1.02d*10**-8*E**2 (JD2411650 - 42500) [8592];
since JD2436470 - see Table.
There is a square term in the ele-
ments given in the Table: -2.7d*10**-8*E**2.
Shape of the light
curve and depths of the Minima vary. According to
[9293] the period of the distortion wave migration is
~ 9.5 yr, the period of the wave amplitude variations
(0 < A <= 0.17m) is ~ 30 yr. According to [9292] the
migration period is nearly half of the value given in
[9293].
RV Lac Mean magnitude varies with the period 550 - 700d.
RW Lac Min II 10.8; DII = 0.024P; Min II - Min I = 0.492P.
RX Lac S7.5/1e. P = 174d (JD2414950 - 29550) [1026];
since JD2436800 - see Table.
RY Lac Oscillations of mean magnitude with P = 300 - 420d
And A <= 0.5m are superimposed by oscillations with
P = 38 - 91d.
SS Lac Probable
member of the open cluster NGC 7209. Min II 10.5;
Min II - Min I = 0.57P; d = 0.008P.
Apsidal motion with P = 1000 yr is possible.
ST Lac Elements should be
checked.
SU Lac P var. Max = 2412748 + 279.10d*E (JD2412700 -
27000) [5707]; Max = 2426972 + 286.74d*E (JD2426900 -
31000); Max = 2431008 + 306.0d*E (JD2431000 - 33150)
[0001]; Max = 2433150 + 319.14d*E (JD2433150 -
42150) [5707]; since JD2442100 -
see Table.
SW Lac Min II 9.31. P var. Min I = 2418943.712 + 0.32071236d*E
(JD2410000 - 19990); Min I = 2420038.621 +
+ 0.32071510d*E (JD2419990 - 25210); Min I =
2430996.525 + 0.32071665d*E (JD2425210 - 33690);
Min I = 2436046.5634 + 0.32072132d*E (JD2433690 -
36755) [5222]; Min I = 2437572.5723 + 0.32072811d*E
(JD2436755 - 40000) [3374]; Min I = 2440467.4592 +
+ 0.32072480d*E (JD2440110 - 40500) [6089]; Min I =
= 2441249.3737 + 0.3207197d*E (JD2440500 - 41600);
[0001]; Min I = 2442697.4039 + 0.3207144d*E (JD
2441600 - 43100) [9295]; Min I = 2443459.7476 +
+ 0.3207216d*E (JD2443100 - 44400) [9297]; Min I =
= 2444856.8064 + 0.3207184d*E (JD2444400 - 44900)
[0001]; since JD2444900 - see
Table.
Shape of the light curve,
depths of minima and heights of maxima vary.
TW Lac d = 0.018P. P var. Min I = 2424387.332 + 3.0374936d*E
(JD2424380 - 34000) [2389]; Min I = 2434049.593 +
+ 3.037520d*E (JD2434000 - 36560) [3115];
since JD2441500 - see Table.
TZ Lac In the region of
the open cluster NGC 7243.
UW Lac Depth of Min II 0.05m; d = 0.028P. P var.
Min I = 2429158.17 + 5.2902d*E (JD2414580 - 29440)
[1813]; Min I = 2429158.17 + 5.290000d*E (JD
2429440 - 35800) [3115]; since JD2436800 -
see Table.
Apsidal motion
is possible [9300].
UY Lac d = 0.022P.
UZ Lac P var?
VX Lac P var. Min = 2424791.488 + 1.0744891d*E (JD
2424700 - 32400); Min = 2432479.477 + 1.0744991d*E
(JD2432400 - 40510); Min = 2440750.971 +
+ 1.0744881d*E (JD2440750 - 43000) [7552];
since JD2443000 - see Table.
VY Lac Min II 10.6. P var? Min I = 2434629.392 + 1.036245d*E
(JD2424700 - 39830) [1804]; since JD
2440080 - see Table.
WY Lac Light va-
riations with P = 850d and A = 1.5m are superimpo-
sed by variations with P = 50d and A = 1m.
XX Lac See TZ Lac.
XZ Lac P var.
AG Lac Min II 14.0.
AR Lac Min II 6.43; Min II - Min I = 0.5018P; dI = 0.045P; DII =
= 0.13P; dII = 0.00P. P var. Min I = 2426624.378 +
+ 1.983244d*E (JD2415300 - 26800) [9309]; Min I =
= 2429535.739 + 1.9832125d*E (JD2426800 - 36000)
[9312]; Min I = 2437018.414 + 1.983252d*E (JD
2436000 - 37500) [0001]; since JD2437500 -
see Table.
There is a square term in the elements
given in the Table: - 5.24d*10**-9*E**2.
Shape of the light curve varies; there is a
distortion wave with A up to 0.13mV migrating in the
direction of decreasing phases with P ~ 2.5 yr. Spect -
rum investigations [1816, 9315, 9316].
AU Lac Min II 12.2; Min II - Min I = 0.53P.
AW Lac Min II 11.2.
BH Lac Hydrogen lines in the spectrum are sharp and deep [3149].
BL Lac Z = 0.07; = +1.0.
Light curve graph [6784].
BM Lac The elements
are valid in the interval JD2425200 - 26250.
BT Lac THere is a square
term in the elements: -0.0004d*E**2. Epoch of Max
brightness is given in the Table. Mean brightness va-
ries in the range 13.8m - 15.2m with P = 654d. Mean
amplitude of the shortperiodical variations is ~ 1.5m.
There occur changes of primaries and secondaries mi-
nima into each other.
BU Lac The main variation
is superimposed by waves with a possible period
- 200d.
CG Lac Min II 14.0.
CM Lac Min II 8.53; DII = 0.12P.
CN Lac Min II 12.6.
In the region of the
open cluster NGC 7209. Not member of the cluster.
CO Lac Min II 10.79.
Apsidal motion with
P = 42.3 yr is observed. There is a periodic term in
The elements given in the Table: -0.0133d cos(157.7deg +
+ 0.0359deg*E).
Min II = 2427534.8439 + 1.5422075d*E + 0.0133d cos(157.7deg +
+ 0.0359deg*E).
CS Lac Min II 9.4.
CZ Lac delta(S) = 1. P var. Max = 2432878.234 + 0.43210346d*E
(JD2428700 - 39400) [1442]; Max = 2443081.309 +
+ 0.4319850d*E (JD2439400 - 43100) [5839]; Max =
= 2444080.122 + 0.432114d*E (JD2443800 - 44100)
[9009]; since JD2445100 - see
Table.
DD Lac VB A (B 9.2m, 69", 16deg). P var. Max = 2421914.178 +
+ 0.19309018d*E - 0.001798d*10**-8*E**2 (JD2421400 -
37600) [5711]; since JD2443000 -
see Table.
According to [9337]
simultaneously the pulsations with the following pe -
riods are observed (the corresponding AB values are
given in the brackets): P1 = 0.193082d (0.080m), P2 =
= 0.197382d (0.034m), P3 = 0.182115d (0.020m), P4 =
= 0.187438d (0.016m), P5 = 0.095109d (0.010m), P6 =
= 0.23583d (0.008m). A var; 0.04m <= A <= 0.12m.
DE Lac delta(S) = 5. P var. Max = 2428807.130 + 0.2536940d*E (JD
2427000 - 33000); Max = 2433005.766 + 0.2536929d*E
(JD2433000 - 39100) [3378]; since JD
2442000 - see Table.
DF LAX [A/H] = 0.2.
DG Lac P var. Min = 2426266.355 + 2.206435d*E (JD2426200 -
40000) [4961]; since JD2440000 -
see Table.
DH Lac P var. Max = 2418240 + 284.8d*E (JD2418000 -
27350); since JD2427300 - see
Table.
DO Lac According to [0085], EA.
EG Lac P > 50d? [5386].
EM Lac Min II 13.09.
EN Lac VB A (B 11.32mV, 27", 345deg; C 9.0mV, 62", 48deg); SB1
(Porb = 12.0968d).
Eclipsing system with a
pulsating primary component of BCEP type. Depth of
Min I 0.05mB. Min I = 2444909.4339 + 12.096816d*E;
D = 0.015P, d = 0.000P. Simultaneously pulsations are
observed with the periods P1 = 0.169170d, P2 = 0.170770d,
P3 = 0.181692d [9346]. The corresponding amplitudes
of pulsations vary. The values of the amplitudes in
B system are as follows: A1 = 0.046m, A2 = 0.024m,
A3 = 0.022m (1952 - 1965); A1 = 0.016m, A2 = 0.010m,
A3 = 0.014m (1977); A1 = 0.010m, A2 = 0.014m, A3 = 0.023m
(1980 - 81). 0.01m <= A <= 0.11m.
EO Lac Min II 12.9; Min II - Min I = 0.485P.
EP Lac Depth of Min II 0.04m.
ER Lac Depth of Min II 0.05m:.
ES Lac Min II 11.6; Min II - Min I = 0.57P.
Apsidal motion is possible: Min II =
= 2433582.95 + 4.459451d*E [9347].
EV Lac VB A (B 12.74mB, 10", 260deg, 1949); mu alfa = - 0.065s,
mu delta = - 0.46". Dark companion (A =
= 0.0206", P = 45 yr, E = 0.5) [9348].
In 1979
sinusoidal light oscillations were observed in the
range 10.20m - 10.27mV: Min = 2444037.576 + 4.378d*E
[9349]. In 1974 - 76 such periodicity was not observed
[9350].
EW Lac Non-radial pulsations with P = 0.7d - 0.8d
are also possible [9351, 9352].
EX Lac d = 0.050P.
FQ Lac A var; P var.
Elements given in the Table are
valid in the intervale JD2427950 - 31700.
FU Lac d = 0.013P.
GS Lac Min II 15.2.
GX Lac Min II 10.23.
HK Lac SB1 (Porb = 24.4284d [9355]).
HM Lac See ER Lac.
HN Lac Min II 14.7.
HR Lac Min II 14.3.
HT Lac In the region of
the open cluster NGC 7209.
HW Lac Min II 14.8.
HX Lac Min II 14.8.
HZ Lac Min II 15.0.
IM Lac Min II 13.2.
IN Lac E?
IP Lac Min II 14.0.
IR Lac Min II 15.4; d = 0.03P.
IT Lac P var.
IU Lac Min II 13.5.
IY Lac Blazhko effect?
IZ Lac Min II 12.7.
KO Lac Min II 14.7.
KP Lac P < 1d.
KR Lac Min II 15.8; dII = 0.05P.
KS Lac Depth of Min II 0.03m.
KU Lac See KS Lac.
Lu Lac Min II 15.32.
LW Lac d = 0.03P. Depth of Min II 0.03m?
LY Lac Min II 12.6.
LZ Lac Min II 12.5.
MO Lac d = 0.04P. See ER Lac.
MP Lac Min II 12.5.
MV Lac Min II 15.0.
MZ Lac Min II 12.1; Min II - Min I = 0.713P. Min II =
= 2433872.702 + 3.158719d*E.
Elements for Min I are given in
The Table.
NN Lac d = 0.02P.
np (usually brigh-
ter) component of a close pair. The range of com -
bined brightness is given in the Table.
NO Lac See KS Lac.
NR Lac Min II 13.4.
Sp (brighter) component of a close pair. The
range of combined brightness is given in the Table.
NU Lac EW?
NW Lac Min II 13.9.
Close binary, the compo-
nents of which are equal in brightness at minimum
light. The range of combined brightness is given in
the Table.
OO Lac Min II 12.8.
OV Lac 150d <= P <= 200d.
OX Lac See EP Lac.
PP Lac Min II 12.0.
PT Lac Min II 15.4.
PZ Lac See TZ Lac.
QQ Lac See TZ Lac.
QU Lac See EP Lac.
V335 Lac Min II 15.8.
V338 Lac In the region of
the open cluster IC 1434.
V339 Lac P = 3.4084964d?
V340 Lac Min II 12.4; Min II - Min I = 0.762P; Min II = 2432858.521 +
+ 19.943102d*E.
Elements for Min I are given in the Table.
V342 Lac Min II 12.9.
V343 Lac Min II - Min I = 0.57P. Depth of Min II 0.03m:.
V344 Lac Min II 13.0. Min I = 2433873.5784 + 0.39222768d*E (JD
2432800 - 35800); since JD2445200 -
see Table.
V345 Lac Min II 11.6; Min II - Min I = 0.340P; DII = 0.040P; dII =
= 0.014P. Apsi-
dal motion is possible.
V347 Lac VB.
V350 Lac VB A (B 9.7m, 66", 94deg); SB 1 (P = 17.755d [9356]).
Min II 6.45 [7468].
Mean magnitude varies. See also
[8933].
V355 Lac Northern component
of a pair.
V360 Lac SB 2 (P = 10d [9357]). Min II 5.93.
V362 Lac VB A (B 13.2m, 1.8", 49deg).
V363 Lac VB A (B 11.3m, F6 III - V:, 6.3", 325deg).
V364 Lac Min II 9.15; Min II - Min I = 0.52P; dI = 0.003P, DII =
= 0.077P, dII = 0.009P.
R Leo P var. Max = 2385112 + 312.43d*E (JD2385100 -
2402500); Max = 2402929 + 314.33d*E (JD2402500 -
11500); Max = 2411416 + 308.93d*E (JD2411500 -
16500); Max = 2416984 + 317.84d*E (JD2416500 -
22500); Max = 2423328 + 312.75d*E (JD2422500 -
27000); Max = 2427081 + 307.40d*E (JD2427000 -
30000); Max = 2437337 + 312.13d*E (JD2430000 -
37500); since JD2437500 - see
Table.
SiO, H2O, OH maser.
S Leo P var. Max = 2420654 + 189.24d*E (JD2420200 -
26100); Max = 2426142 + 185.92d*E (JD2426100 -
28100); since JD2428100 - see
Table.
T Leo SB 1 (Porb = 0.05881873d [9304]).
V Leo H2O maser.
W Leo P var. Max = 2434651 + 385.41d*E (JD2409500 -
35000); since JD2437500 - see
Table.
OH maser.
Y Leo P var. Min = 2422372.520 + 1.6860978d*E (JD2418000 -
23500) [2389]; Min = 2422372.5368 + 1.68607314d*E
(JD2423500 - 38600) [9307]; since JD
2438600 - see Table.
There is periodic term in the ele -
ments given in the Table: + 0.00375d*sin(0.21487deg*E +
+ 141.7deg). Depth of Min II 0.1m IR.
RR Leo delta(S) = 7.1. P var. Max = 2430440.3385 + 0.45238172d*E +
+ 1.963d*10**-10*E**2 (1898 - 1977) [8299]; since
JD2441400 - see Table.
RT Leo Min II 10.5.
RW Leo P var. Before JD2440800 Min = 2424993.458 +
+ 1.6825365d*E [3115]; since JD2440800 -
see Table.
RX Leo delta(S) = 6.8.
SS Leo P var. Max = 2415485.723 + 0.62633242d*E (JD
2414000 - 22000) [0752]; since JD2422000 -
see Table.
[Fe/H] = - 1.59.
ST Leo (k - b)2 = 0.08.
SZ Leo P var. Before JD2442500 Max = 2425331.400 +
+ 0.5340833d*E [4157]; since JD2442500 -
see Table.
Light curve shape var?
TU Leo In light minimum: +0.22 <= B - V <= +0.56,
U - B = -0.08, J = 14.05m, K = 12.91m.
Single reliable outburst.
TV Leo P var. Max = 2419852.318 + 0.6728362d*E (JD
2419000 - 28000) [0001]; since JD2437000 -
see Table.
(k - b)2 = -0.01.
TX Leo VB A (B 7.8m, 2", 157deg, 1971);
A binary according to lunar occul-
tation data: ro = 0.0005".
The
range of combined brightness is given.
Min II 5.69; DII = 0.19P; Min II - Min I = 0.550P.
TY Leo Elements need
confirmation.
UU Leo Min II 11.5. P var. Since JD2430000 -
see Table.
UV Leo Min II 9.49; d = 0P014. P var. Before JD
2434000 Min I = 2425574.302 + 0.60008516d*E [7554];
since JD2434000 - see Table.
UX Leo Min II 10.4.
Moments of Min by
BBSAG contradict the tabulated elements.
UZ Leo Min II 10.12. P var, nonlinear
term: + 2.8d*10**-12*E**2.
XX Leo Min II 11.4. Period
should be checked.
XY Leo Min II 9.80. P var. Min = 2435195.66306 + 0.2841091d*E
(JD2434000 - 36500) [3392]; Min = 2437376.465 +
+ 0.28409592d*E (JD2436500 - 40000) [0001]; Min =
= 2441005.5364 + 0.28410727d*E (JD2441000 - 44000)
[9084]; since JD2444000 - see
Table.
The light curve shape var.
XZ Leo Min II 11.1.
AB Leo Epoch of Min is given.
According to [1853], Max = 2428880 +
+ 103.2d*E (JD2414600 - 19000, 2428000 - 31600);
During other time intervals
cycles 75d - 125d.
AD Leo mu = 0.49", P = 265deg; pi = 0.20".
X-ray and radio source.
Astrometric binary?
AF Leo H2O maser.
AM Leo VB A (B 10.64m, 11", 270deg). Min II 9.83.
AP Leo Min II 9.88. P var. Min = 2414986.868 + 0.430350d*E
(JD2414700 - 18600); since JD2418600 -
see Table.
Light curve shape var.
AQ Leo Elements for fundamental mode pulsations (P0)
see Table.
For the first overtone: P1 var?;
P1 = 0.4101369d (1929 - 1969); P1 = 0.410130d (1957 -
1969); during 1973 - 1975 Max1 =
= 2441766.486 + 0.4101487d*E. delta(M0) = 0.23m, delta(M1) = 0.46M.
AU Leo Vr = + 7545 km/s. Varia-
bility is doubtful.
BB Leo [Fe/H] = -1.32.
BL Leo Min II14.4. P var. Since JD2442000 -
see Table.
BV Leo Min II 16.1.
BW Leo Min II 15.4.
BX Leo [Fe/H] = -1.23.
BZ Leo Min II 15.8.
CD Leo Light curve shape var.
CE Leo Min II 12.5. P var?
Min by BBSAG contradict the tabulated ele -
ments.
CN Leo Mu = 4.7", P = 235deg; pi = 0.41".
Soft X-ray source, radio
source.
CW Leo Dust envelope, 6"*4".
Molecular radioemis-
sion: SiO, SiS, HCN, HC3N, CO, H2O, NH3, etc.
Polarization in I
band up to 24%.
CX Leo VB A (B 12.3m, 132deg); SB (Porb = 12685.4d).
CY Leo mu = 0.307", P = 141.3deg; pi = 0.022".
Outside flares delta(m) < = 0.036m; P = 600s, 822s, 1638s
[6209].
A single
strong flare with delta(M) = 0.61m in blue light of 10 Min
duration was observed [6141], which is attributed by
several authors to the presence of a red flaring com -
panion.
DE Leo P = 1.2d - 2.0d?
DG Leo VB B (A 6.6m, A 8IV, SB 2, Porb = 4.15d; B 6.9m, 0.271",
211.2deg, 1980, Porb ~ 200yr).
The range of the bom-
bined brightness is given.
DH Leo SB 1, Porb = 1.070354d.
DK Leo mu alfa = -0.097", mu delta = - 0.214".
R LMi SiO, H2O, OH mazer.
T LMi Min II 10.97. P var. Min I = 2420573.698 + 3.019889d*E
(JD2420200 - 25000); Min I = 2423856.323 +
+ 3.0199336d*E (JD2423800 - 35500); since
JD2438400 - see Table.
U LMi 1m <= A <= 3.3m.
Periodicity sometimes breaks down.
V LMi delta(S) = 5.7.
Y LMi P var. Max = 2428636.322 + 0.52443938d*E + 0.0597d*
*sin(0.0657deg*E + 27.2deg) (JD2425250 - 28500); Max =
= 2428636.348 + 0.5244564d*E (JD2428500 - 30000)
[1856]; mean elements
for interval JD2432200 - 38900 are given in the
Table; in this interval the period changed with the
cycle of ~ 2100d.
Blazhko effect
with the period 33.4d [1856]; 07m <= A <= 1.9m, 0.19P <=
<= m - M <= 0.44P.
RT LMi Min II 11.7.
RU LMi Spectrum description [9326].
RW LMi VB A (B 15.5m B, 9", 10deg). 0.3m - 2.6m K, 7.64m - 10.71m,
9.7m - 14.6m R, 14.1m - 18.1m B, 14.8m - 18.6m U.
Mean brightness varies. Gaseous-dust circumstel-
lar envelope. CO emission. Spectrum description
[9327].
RY LMi VB A (B 16.1m, dM2, 15", 126deg); mu = 0.14", P = 264deg.
P0 = 215.197388s, P0 = 5.6s*10**-14/s, A0 = 0.0440m;
P1 = 304.4s, A1 = 0.0150m; P2 = 271.0s, A2 = 0.0134m;
P3 = 107.6s, A3 = 0.0032m; P4 = 126.2s, A4 = 0.0028m;
P5 = 119.8s, A5 = 0.0026m.
Mean brightness varies by 0.05m.
R Lep P var. Max = 2398883 + 436.44d*E (JD2398000 -
2412000); Max = 2412849 + 418.04d*E (JD2412000 -
23000); Max = 2423300 + 441.38d*E (JD2423000 -
36000); since JD2436000 - see
Table.
A var; 5.5m <= Max <= 9.5m (Possible period is more than 40 years
[3402]).
S Lep Mean
magnitude varies with the cycle of 890d. H2O
maser.
T Lep SiO maser.
U Lep P var. Max = 2425084.431 + 0.58147098d*E (JD
2411000 - 25090); Max = 2425084.431 + 0.58147377d*E
(JD2425080 - 37700) [3403]; since JD
2436600 - see Table.
delta(S) = 8.5; (k - b)2 = 0.00.
V Lep Min II 9.9.
Z Lep Min II 12.0:.
RR Lep Min II 10.4.
RS Lep Min II 9.96.
RU Lep P var?
RZ Lep S 4/4.
SS Lep SB 2 (Porb = 258.2d [9363]).
SY Lep VB A (B 15.2m: V, 18", 270deg).
S Lib P var. Max = 2405692 + 192.14d*E (JD2402700 -
24000); Max = 2424141 + 194.74d*E (JD2424000 -
30500); Max = 2431900 + 190.34d*E (JD2430500 -
37200); Max = 2439203 + 197.61d*E (JD2437200 -
39300); since JD2441000 - see
Table.
Mean value of the period is given in the Table.
A var (1.8m <= A <= 5m).
W Lib P var. Max = 2412272 + 203.76d*E (JD2412000 -
28500); Max = 2428573 + 201.48d*E (JD2428500 -
34000); since JD2434000 - see
Table.
X Lib P var. Max = 2423500 + 165.75d*E (JD2413000 -
25000); since JD2425000 - see
Table.
Y Lib P var. Max = 2413452 + 275.7d*E (JD2413400 -
22000); Max = 2422273 + 272.5d*E (JD2422000 -
28000) [0458]; Max = 2434921 + 277.04d*E (JD
2428000 - 35000); since JD2435000 -
see Table.
Z Lib P var. Max = 2417736 + 294.5d*E (JD2407100 - 17800);
since JD2424400 - see Table.
RR Lib P var. Max = 2409699 + 277.4d*E (JD2409600 -
15600); Max = 2416345 + 273.2d*E (JD2416300 -
19700); Max = 2421027 + 278.6d*E (JD2421000 -
27150) [0458]; since JD2427150 -
see Table.
RS Lib P var. Max = 2413396 + 217.2d*E (JD2413300 -
20000); Max = 2420110 + 219.6d*E (JD2420000 -
27500) [0458]; Max = 2429078 + 215.6d*E (JD2427500 -
35000); Max = 2438196 + 219.9d*E (JD2435000 -
42600); since JD2441700 - see
Table.
RT Lib P var. Max = 2413776 + 254.21d*E (JD2413000 -
19000); since JD2419000 - see
Table.
RU Lib P var. Max = 2413363 + 312.0d*E (JD2413300 -
16200); Max = 2416807 + 322.5d*E (JD2416800 -
21000); Max = 2421309 + 317.0d*E (JD2421300 -
24200); Max = 2424804 + 311.5d*E (JD2424800 -
29800) [0458]; Max = 2434909 + 319.9d*E (JD2429800 -
35000); since JD2437700 - see
Table.
RV Lib Min II 9.44.
RX Lib [A/H] = -0.5. P var. Max = 2430913.6 + 24.950d*E
(JD2425000 - 36300) [0266]; since JD
2436300 - see Table.
SS Lib Min II 10.8; d = 0.030P.
ST Lib VB A (B 14m, 14", 0deg).
TV Lib delta(S) = 2.5.
TY Lib d = 0.019P.
UW Lib [Fe/H] = - 0.25.
VV Lib P var. Max = 2424268.474 + 0.4781418d*E (JD
2419800 - 2425000); since JD2425000 -
see Table.
VW Lib Observations given in
[0293] contradict the elements given in the Table.
VY Lib P var? [3506].delta(S) = 6.
VZ Lib Min II 10.55; dI = 0.000P; dII = 0.005P. P var. Min I =
= 2429022.227 + 0.358053d*E (JD2428600 - 30400)
[9368]; Min I = 2430899.223 + 0.358448d*E (JD
2430400 - 32400) [2532]; since JD2444330 -
see Table.
YZ Lib Min II 12.9.
AA Lib P var?
The elements are valid in the interval
JD2427800 - 29600.
AP Lib Z = 0.0486.
AQ Lib [Fe/H] = -0.60.
BT Lib Min II 12.3.
CG Lib [Fe/H] = -1.82. P var. Max = 2438592.287 +
+ 0.3068674d*E (JD2427800 - 39600) [7557];
since JD2439600 - see Table.
EH Lib delta(S) = 0. 9.35m <= Max < = 9.49m V; Max (A) = 2442162.556 +
+ 0.273778d*E [9336].
ES Lib Min II 7.33.
EU Lib 70d <= P <= 90d.
FI Lib 90d <= P <= 110d.
FS Lib OH emission.
FX Lib Spectrum description 6167,
[9371].
del Lib VB A (B 11.3m, 9", 351deg; C 12.80m, 67", 90deg); Min II
4.98. P var?
S Lup VB A (B = X Lup, 13", 176deg). P var. Max = 2411950 +
+ 347.81d*E (JD2411950 - 14000); Max = 2414040 +
+ 339.31d*E (JD2414000 - 19000); Max = 2419135 +
+ 345.12d*E (JD2419000 - 26000); Max = 2426038 +
+ 336.60d*E (JD2426000 - 29500); Max = 2429743 +
+ 345.15d*E (JD2429500 - 35000); since JD
2437600 - see Table.
X Lup VB B (see S Lup).
Y Lup P var. Max = 2424691 + 408.15d*E (JD2423000 -
25500); Max = 2425503 + 394.81d*E (JD2425500 -
30250); Max = 2430641 + 407.75d*E (JD2430250 -
35000); since JD2437900 - see
Table.
RU Lup Sometimes varies quasiperiodically: P1 = 3.5457d, P2 =
= 3.8375 [2412]. H2O maser.
RY Lup Quasiperiodicity: P = 3.7609d
[9366].
SX Lup Min II 11.8.
UX Lup [A/H] = -0.9. P var. P = 16.2403d (JD2411526 -
14040); P = 16.2065d (JD2414040 - 24016); P =
= 16.2492d (JD2424016 - 25638); P = 16.1794d (JD
2425638 - 26449); P = 16.2241d (JD2426449 - 29693)
[5387].
VV Lup Close northern compa-
nion.
VZ Lup P var? Light curve shape
var?
CX Lup Min II 12.8.
CY Lup High Max every 360d, es-
pecially faint Min 80d before these high Max.
DG Lup Min II 15.1.
EL Lup VB.
ER Lup P2 = 140d.
FK Lup Min II 10.7:.
FR Lup Deep Min II.
FT Lup Min II 9.98. dI = 0.025P?, dII >= 0.066P. P var.
Before JD2439300 Min I = 2427987.310 + 0.470089d*E
[3948]; since JD2445000 - see
Table.
All the observations are well represented
also by the elements: Min I = 2445061.834 +
+ 0.470083D*E - 0.114d*10**-9*E**2 [9360].
Light curve shape var?
FV Lup Min II 11.2.
GG Lup Min II 5.8.
GN Lup VB A (B 10.2m vis, 10", 98deg).
GO Lup Relatively short P.
GW Lup In the dark nebula Barnard 228.
HK Lup B - V: +1.23, +1.46.
HL Lup 2U 1543 - 47.
HM Lup B - V: +1.12.
HN Lup B - V: +1.55, +1.68.
HO Lup B - V: + 0.70, + 0.81.
alf Lup VB A (B 14.0m, 27.6", 232deg, 1901).
Soft X-ray
source.
P2 = 3.145d is possible [8417].
del Lup Less pro -
bable variant of elements: Max = 2441045.160 +
+ 0.14273*E.
R Lyn S 4/5E - S 6/6 - .
S Lyn VB A (B 14m, 12.6", 155deg). P var. Max = 2414564 +
+ 300.26d*E (JD2414500 - 27400); Max = 2434241 +
+ 294.42d*E (JD2427400 - 35100); Max = 2440225 +
+ 300.44d*E (JD2435100 - 40220); since JD
2440220 - see Table.
T Lyn P var. Max = 2425012 + 419.0d*E (JD2412800 - 34700);
since JD2434700 - see Table.
U Lyn H2O, OH emission. P var. Max = 2417168 +
+ 440.3d*E (JD2417100 - 26000) [0458]; Max =
= 2435908 + 432.05d*E (JD2426000 - 36000); Max =
= 2439898 + 447.1d*E (JD2436000 - 40000);
since JD2440000 - see Table.
V Lyn Cycles 55d and 87d replace
one anotHer. Mean brightness varies.
Y Lyn SB.
RR Lyn VB A (B 10m, 50"). Min II 5.90; Min II = 2438051.3115 +
+ 9.945074d*E; E = 0.081; Min II - Min I = 0.45P (JD
2437700).
RW Lyn [Fe/H] = -1.37.
RZ Lyn Min II 10.8.
SW Lyn Min II 9.65; dI = 0.038P. P var. Min I = 2425643.323 +
+ 0.6440661d*E (JD2425640 - 35850) [2742]; Min I =
= 2438795.8016 + 0.6440520d*E (JD2438380 - 840)
[9387]; Min I = 2440614.0107 + 0.6440729d*E (JD
2439500 - 40620) [0001]; Min I = 2442786.4493 +
+ 0.6440677d*E (JD2440650 - 42790) [7292];
since JD2442780 - see Table.
SX Lyn Min II 10.1. P var. Min I = 2428636.375 + 2.0225615d*E
(JD2427400 - 34700) [0519]; Min I = 2442561.424 +
+ 2.0225172d*E (JD2442400 - 44000); since
JD2444000 - see Table.
SZ Lyn SB (Porb = 1146d, E = 0.26 [9388]). delta(S) = 0.
There is a perio-
dical term in the elements: - 0.00573d cos 2pi (EP0/P1 +
+ 0.007); P0 = 0.120534920d, P1 = 1150d.
Amp-
litude and shape of the light curve vary.
TT Lyn delta(S) = 7.
TV Lyn [Fe/H] = - 0.99.
TW Lyn delta(S) = 10. P var. Max = 2418676.804 + 0.4817201d*E (JD
2418670 - 20155); Max = 2420155.685 + 0.4816929d*E
(JD2420155 - 27480); Max = 2427479.359 +
+ 0.4817481d*E (JD2427480 - 28630); Max =
= 2428627.310 + 0.4818529d*E (JD2428620 - 37800)
[2819]. Since JD2445000 - see
Table.
TZ Lyn Epoch of Min brightness
is given.
UU Lyn Min II 11.82.
UV Lyn Min II 9.78.
UZ Lyn VR var (P = 0.065d [9392]).
VV Lyn VB A (B 11.76m, 38.6",354deg); SB; mu alfa = -0.0285S,mu delta =
= -0.274".
VW Lyn P1 = 590s, P2 = 260s [9393].
S Lyr P var. Max = 2416186 + 432.01d*E (JD2415700 -
20100); Max = 2420961 + 445.83d*E (JD2420900 -
26500); Max = 2426748 + 429.01d*E (JD2426500 -
30700); Max = 2432357 + 441.88d*E (JD2432000 -
34600); since JD2442500 - see
Table.
U Lyr VB A (B 13.0m, 9.4", 182deg). P var. Max = 2418345 +
+ 459.22d*E (JD2418000 - 27000); since JD
2432000 - see Table.
V Lyr OH maser.
W Lyr P var. Max = 2415578 + 198.39d*E (JD2413000 -
19000); Max = 2420322 + 194.99d*E (JD2419000 -
25500); Max = 2431326 + 198.97d*E (JD2427000 -
31500); Max = 2432494 + 195.11d*E (JD2431500 -
36500); since JD2437500 - see
Table.
Y Lyr delta(S) = 0.8.
Z Lyr P var. Max = 2418150 + 285.07d*E (JD2417500 -
22200); Max = 2423600 + 291.37d*E (JD2422200 -
29500); Max = 2430000 + 284.00d*E (JD2429500 -
36800); since JD2436800 - see
Table.
RR Lyr mu alfa = -0.11", mu delta = -0.19". [Fe/H] = -1.14; delta(S) = 6.
Blazhko effect of variable
amplitude (practically to complete disappearance of
blazhko effect); Pi = 40.8d. Variations of Max light
phase up to 0.14P; magnitude in Max var in the range
up to 0.6m, that in Min var in the range up to 0.1m
[3418].According to [7270], a cycle ~ 4 yr is present
in blazhko effect amplitude changes; at the end of
the cycle the blazhko effect phase changes abruptly
by 0.25Pi. Magnetic field strength varies with the
pulsational period [9339].
P var. Max = 2414856.480 + 0.56682069d*E (JD
2414800 - 18800); Max = 2421854.052 + 0.56685169d*E
(JD2418800 - 26500) [9379]; Max = 2426571.3828 +
+ 0.56684333d*E (JD2426500 - 32500) [9338]; Max =
= 2438215.9492 + 0.566830d*E (JD2438000 - 41000)
[5238]; Max = 2438215.9492 + 0.56683313d*E (JD
2441000 - 42900) [9338]; since JD2442900 -
see Table.
RS Lyr P var. Max = 2415566 + 299.38d*E (JD2415000 -
24000); Max = 2425176 + 308.08d*E (JD2424000 -
37200); since JD2437200 - see
Table.
RT Lyr P var. Max = 2437022 + 250.85d*E (JD2415000 -
39000); since JD2439000 - see
Table.
RU Lyr P var. Max = 2415983 + 370.70d*E (JD2415900 -
33000); Max = 2433035 + 363.0d*E (JD2433000 -
41000); since JD2441000 - see
Table.
RV Lyr D = 0.015P. P var. Min = 2415949.7096 + 3.599007d*E
(JD2412185 - 16000); Min = 2415949.7096 +
+ 3.599046d*E (JD2416000 - 21400) [0001]; Min =
= 2432015.671 + 3.5989845d*E (JD2421400 - 32000);
Min = 2432015.671 + 3.5990235d*E (JD2432000 -
39300) [9085]; since JD2442000 -
see Table.
RW Lyr OH, H2O maser.
RX Lyr P var. Max = 2416226 + 249.94d*E (JD2415000 -
28800); since JD2428800 - see
Table.
RZ Lyr P var. Max = 2416415.360 + 0.51127069d*E (JD
2413000 - 19000) [0001]; Max = 2426161.4375 +
+ 0.51124948D*E (JD2426000 - 38000) [0323];
since JD2438000 - see Table.
Blazhko
effect, height of Max varies: 10.6m - 10.9m, Max (delta(m)) =
= 2430904.3 + 116.654d*N + 0.01034d*N**2; Min (delta(m)) -
- Max (delta(m)) = 59.3d [3419].
[Fe/H] = -1.69; delta(S) = 10.0.
SS Lyr P var. Max = 2421695 + 350.48d*E (JD2416000 -
22500); Max = 2429991 + 355.22d*E (JD2429000 -
38000); since JD2438000 - see
Table.
SZ Lyr According to [5750], during JD2434665 -
35044 the amplitude was twice smaller than usual
(due to the depth of Min), and a temporary phase
shift by 0.5P occured.
TT Lyr d = 0.010P; Min II 9.44.
TW Lyr VB A (B 15.2m pg, 14".70deg, 1912).
TY Lyr P var. Max = 2419285 + 336.49d:*E (JD2419000 -
23700); Max = 2423985 + 329.79d*E (JD2423700 -
31250); since JD2438600 - see
Table.
TZ Lyr VB A (B 12.29m, 2.54", 2.5deg). Min II 11.05. P var.
Min I = 2420669.480 + 0.5288234d*E (JD2420000 -
38000); since JD2438000 - see
Table.
UX Lyr B - V: +0.11, +0.47.
UZ Lyr d = 0.012P:. P var. Min = 2424268.474 + 1.891253d*E
(JD2422500 - 25500) [2087]; since JD
2425500 - see Table.
AA Lyr Min II 13.5.
AH Lyr d = 0.03P. Min II 12.1.
AK Lyr Min II 12.9.
AL Lyr P var. Max = 2427865.82 + 12.9837d*E (JD2414800 -
28000) [0001]; Max = 2432889.03 + 12.98047d*E (JD
2428000 - 35500) [4427]; since JD2435500 -
see Table.
AQ Lyr P var. Max = 2425301.592 + 0.3571721d*E (JD2425300 -
29000); Max = 2428944.739 + 0.3571285d*E (JD
2429000 - 30200); Max = 2430158.976 + 0.3571611d*E
(JD2430200 - 33900); Max = 2433909.178 +
+ 0.3571861d*E (JD2433900 - 35700);
during JD2435700 - 37800 - see Table.
Blazhko effect? According to visual observations,
0.4m <= delta(m) <= 1.2m.
AY Lyr Cycles of supermaxima
188.9d - 212.8d.
Superhumps period: Ps = 0.07552d
[6249].
BF Lyr P var. Max = 2425296 + 130d*E (JD2425300 - 800);
During JD2429045 - 570 -
see Table.
BH Lyr P var. Max = 2413712.358 + 0.6129028d*E (JD
2413712 - 27927); Max = 2434472.547 + 0.6128941d*E
(JD2434472 - 36102); since JD2436423 -
see Table.
BQ Lyr delta(S) = 0:.
BV Lyr d = 0.025P.
CC Lyr P var. Max = 2433182.7 + 24.028d*E (JD2426100 -
33400); Max = 2437078.8 + 24.200d*E (JD2433400 -
37100) [0001]; Max = 2439418.5 + 24.185d*E (JD
2437100 - 39420) [5644]; since JD2440400 -
see Table.
Light curve shape var?
[A/H] = -2.2.
CV Lyr Possible superposition of
P2 = 135d.
CX Lyr P var. Max = 2418596.111 + 0.616689d*E (JD
2414880 - 20000); Max = 2427696.396 + 0.616669d*E
(JD2427530 - 30610); since JD2433000 -
see Table. delta(S) = 7:.
DD Lyr P var. Max = 2425494.334 + 0.372610d*E (JD
2418900 - 27600) [0001]; since JD2427600 -
see Table.
DF Lyr Min II 13.4.
DI Lyr P var. Max = 2437160.310 + 0.4174486d*E (JD
2437160 - 39293); Max = 2439293.468 + 0.4178451d*E
(JD2439293 - 40768); since JD2440768 -
see Table.
DN Lyr P2 = 600d.
DR Lyr [Fe/H] = - 1.41; delta(S) = 7.4.
DU Lyr Min II 13.3.
EN Lyr B - V: + 0.40. + 0.43. P var. delta(m) var.
EP Lyr Max I ” = 0.20P; Min II 10.36m - 10.58m, ” = 0.50P; Max II
10.01m - 10.10m, ” = 0.70P.
Secondary oscillations: P2 = 45.1d, P3 = 7067d [9354].
EW Lyr P var; nonlinear term:
+ 0.00210d*10**-6*E**2 (JD2426500 - 45500);
since JD2442000 the obser-
vations are represented also by the elements: Min =
= 2445597.391 + 1.948763d*E [7037, 0001].
EX Lyr [Fe/H] = - 0.63; delta(S) = 2.5.
EZ Lyr VB A (B 12.3m, 14", 302deg, 1934). P var. Since
JD2426577 - see Table. delta(S) = 7.1.
FG Lyr VB A (B 14m, <10"). d = 0.035P. P var?
FH Lyr P var?
FK Lyr The identification with HDE 337663(G5) [0021] is
wrong.
FL Lyr Min II 9.52, DII = 0.05P.
FN Lyr B - V: +0.15, +0.48.
FO Lyr Min II 13.7.
GY Lyr The elements describe the brightest ma-
ima. Between them iHere are 2 - 3 waves of smaller
amplitude. Red.
HP Lyr Min II 11.0.
HQ Lyr P var, periodic term:
+ 30d sin(8deg*E).
HT Lyr Min II 13.3.
HY Lyr Min II 14.1.
IK Lyr Blazhko effect?
IL Lyr According to [0569], Max = 2429375.519 +
+ 0.377620d*E, M - m = 0.14P:.
IO Lyr delta(S) = 3.
IP Lyr Min II 13.3.
IW Lyr Min II 13.3.
IY Lyr Min II 14.1.
KM Lyr Blazhko effect: Pi = 30d, 0.14P <=
<= M - m <= 0.20P.
KP Lyr ADS 11423 C (A 8.5m, B 9.7m; AB - C 77", 208deg; D 13.1m,
C - D 14", 61deg, 1904). P2 = 1300d is pos -
sible.
KR Lyr P var. The light curve shape
var.
KT Lyr Min II 14.9.
KX Lyr delta(S) = 0.
LQ Lyr [Fe/H] = -1.39; delta(S) = 7.2.
LR Lyr P var? [Fe/H] = -1.41; delta(S) = 7.4.
LT Lyr Ra-
pid variation (0.5m in an hour ) were observed.
LX Lyr delta(S) = 8:.
LZ Lyr P var. Min = 2425347.565 + 1.611143d*E (JD2425347 -
32119) [0569]; since JD2442870 -
see Table.
MN Lyr Min II 14.1.
MR Lyr Alternative P = 0.66d:.
MS Lyr P < 0.5d?
MT Lyr Min II 16.2.
MV Lyr SB (Porb = 0.1336d [9373]).
Quasiperiodic
fadings of different amplitude: Min = 2425558 + 455.5d*E
(JD2425500 - 30100); Min = 2430113 + 325.3d*E (JD
2430100 - 36900); Min = 2436944 + 357.8d*E (JD
2436900 - 44100) [9372].
After JD2444100 the mean brightness
level became fainter by 5m; outbursts with an ampli -
tude up to 3m of 1 - 2 months duration are observed
[9404]. During the bright level of light, flickering up
to 0.4m in 5 Min in U bAnd is observed [0365]. Soft
X-ray source.
B - V: 0.00 +- 0.40; U - B: -0.86 + -1.30.
MW Lyr P var. Max = 2429521.386 + 0.3978817d*E (JD
2427700 - 36000); since JD2436000 -
see Table.
Blazhko effect: Pi = 33.3d;
The amplitude varies by
0.6m.
MZ Lyr Min II 14.0.
NV Lyr d = 0.02P:.
NW Lyr P var. Max = 2436483.323 + 1.6012330d*E (JD2414500 -
36400) [3506]; since JD2436400 -
see Table.
B - V: +0.38, +0.86.
NY Lyr Min II 13.1.
NZ Lyr O - C vary harmonically with an amplitude +- 0.01d,
Pi ~ 2500P.
OQ Lyr VB (B 12.1m vis, 5.3", 175deg, 1930).
OS Lyr 40d <= P <= 60d. P2 = 400d - 500d is superimposed.
PQ Lyr d = 0.014P; Min II 14.9.
PS Lyr d = 0.02P:; Min II 11.4.
PU Lyr Close companions sf, s.
PV Lyr d = 0.03P:.
PY Lyr Min II 13.4. P var. Min I = 2434980.4372 + 0.38576671d*E
(JD2432700 - 36900) [4248]; since JD
2442500 - see Table.
QQ Lyr Min II 14.6.
QT Lyr Min II 14.6.
QU Lyr Min II 13.1.
V335 Lyr Large scat-
ter in the light curve.
V336 Lyr P var. Min = 2429965.283 + 1.9049105d*E (JD
2429370 - 31590); during JD2438930 -
40010 - see Table.
V337 Lyr See V335 Lyr.
V348 Lyr Min II 16.8.
The elements are valid during JD2444023 - 45232.
V350 Lyr P var. The ele-
ments are valid during JD2438280 - 45232.
V355 Lyr The elements
are valid during JD2429322 - 45232.
V356 Lyr VB A (B 17.5m, 10", 120deg, [0001]).
V361 Lyr Min II 15.3, Max II 14.7, Max II - Min I = 0.70P.
The elements are valid
during JD2433776 - 45232).
V374 Lyr Faint companions np, sf.
V380 Lyr Faint close companion nf.
V385 Lyr Faint close companion sf.
V388 Lyr No brighte-
nings were observed during JD2438322 - 39289.
V389 Lyr The elements
are valid during JD2438322 - 40007.
V390 Lyr The elements
are valid during JD2439913 - 40007.
V401 Lyr Min II 14.4:. The
period may be spurious.
V403 Lyr P var?, Pi = 500 P?
V404 Lyr Min II 12.4.
V406 Lyr Min II 13.0.
V409 Lyr P var? The ele-
ments are valid during JD2434500 - 40000.
Blazhko effect?
V411 Lyr Min II 14.4. Alternatively RRC (P =
= 0.291315d).
V412 Lyr Min II 14.1; Min II - Min I = 0.48P.
V413 Lyr Min II 14.8?
V415 Lyr Cycle <= 150d.
V417 Lyr Min II 16.2. P var?
V418 Lyr P var. The ele-
ments are valid during JD2437100 - 40400.
V423 Lyr Min II 15.5. P var?
V424 Lyr See IK Lyr.
V428 Lyr Min II 14.3. Apsidal mo-
tion?
V429 Lyr Min II 14.8?
V431 Lyr Min II 15.1.
V435 Lyr Possibly ew with twice longer P. P may
be spurious.
V462 Lyr P var? The
elements are valid during JD2439913 - 40007.
V467 Lyr Min II 12.9.
JD2415288 - 43287;
The elements
are valid during JD2415288 - 43287; large scatter
on the light curve. According to [9412], during JD
2443424 - 44165 the light variation range is 12.4m -
12.6m pg, the elements are not valid.
V470 Lyr U = 0.40", p = 7deg. P1 = 738.6s, P2 = 557.4s, P3 = 318.0s,
P4 = 291.9s, P5 = 259.1s.
V473 Lyr P var, delta(m) var. According to [9413], P =
= 1.490795d + 1.22d*10**-6*(JD - 2443600)/365.25d.
Cyclic P variations: P alfa =
= 1178.5d; Pt = 2655d.
delta(m) varies with the pe-
riod P alfa; P4 = 1063.5d may be traced in the variations
of Vr.
0.06m <= delta(m) <= 0.36m.
V474 Lyr P2 = 76d.
V477 Lyr The central
star of planetary nebula Abell 46. Strong reflec-
tion effect.
Depths of minima: Min I 1.42m B,
Min II ~ 0.1m B.
alf Lyr IR excess.
bet Lyr ADS 11745 A (B 8.6m, B7V, 46", 149deg; C 13.0m, 47",
248deg). Min II 3.85. P var.
Nonlinear terms: + 3.883d*10**-6*
*E**2 - 0.10d*10**-10*E**3.
Light curve shape var.
Radio- and X-ray source. IR excess.
del 2 Lyr Open cluster delta**2 Lyr
member [2505].
R Men Sometimes P = 120d;
Sometimes P = 240d.
T Men See RS Men.
THere is a sguare term in the elements:
+ 8.1d*10**-6*E**2.
U Men VB A (B 10.4m, 0.6", 71deg, 1935.3). A var (0.8m <= A <= 2.9M).
P var. Max = 2416927 + 426.9d*E (JD2415200 - 17400)
[0207]; since JD2417400 - see
Table.
V Men Epoch corresponds to the middle of
the light curve ascending branch.
W Men The member
of the Large Magellanic Cloud.
RR Men Min II 12.1.
RS Men In the Large Magellanic Cloud region; not
a member of the Cloud.
RT Men See RS Men.
RU Men See RS Men.
RV Men See RS Men.
RW Men See RS Men.
TU Men Porb = 0.1176d [9376]. Superhump
Period Ps = 0.12625d [4772].
TY Men Min II 8.47; d I = 0.00P, d II = 0.07P.
Shape of the light curve varies.
TZ Men Min II 6.36.
UX Men Min II 9.47; Min II - Min I = 0.50045P.
One of the components may be a physical variable.
WY Men In the region of the NGC 1841 globular clus-
ter; not a member of the cluster. In the halo of the
magellanic clouds system.
WZ Men See WY Men.
XX Men See WY Men.
XY Men See RS Men. Min II 10.88; dI = 0.05P; dII = 0.00P.
XZ Men There
are there oscillations simultaneously: P1 = 0.1083d
(A1 = 0.0094m B), P2 = 0.0855d (A2 = 0.0082m B), P3 =
= 0.0955d (A3 = 0.0058m B); P2/P1 = 0.789.
iot Men Min II 6.05.
R Mic P var. Max = 2413373 + 138.60d*E (JD2413300 -
29600) [0458]; Max = 2432745 + 137.43d*E (JD
2429600 - 34700); Max = 2435091 + 140.84d*E (JD
2434700 - 37800); since JD2437800 -
see Table.
S Mic P var. Max = 2413499 + 214.5d*E (JD2413500 -
15900) [0458]; Max = 2432102 + 208.23d*E (JD
2422700 - 32200); since JD2432200 -
see Table.
U Mic OH, H2O emission.
V Mic See U Mic.
Y Mic Mean brightness varies.
Z Mic (k - b)2 = 0.12; delta(S) = 4.
RR Mic [A/H] = - 1.4. P var. Max = 2433032.96 + 31.78175d*E
(JD2415000 - 35300) [2747]; since JD
2443600 - see Table.
RY Mic P var?
Elements given in
the Table represent observations in the interval JD
2436100 - 40210.
According to [0085] Max = 2428670 +
+ 190d*E.
RZ Mic Min II 11.2.
TV Mic Min II 12.4.
UZ Mic Min II 12.4.
VW Mic In the interval JD2436600 - 840)
Max = 2436807.248 + 0.35620d*E. Since JD
2442600 - see Table.
WY Mic P = 0.511427d? [0001].
XZ Mic In the interval JD2436670 - 840 Max =
= 2436731.480 + 0.449208d*E. Since JD
2442630 - see Table.
ZZ Mic (k - b)2 = 021; delta(S) = 0. P var? Max = 2437192.3131 +
+ 0.0671786d*E (JD2437180 - 460) [4308]; Max =
= 2439320.2162 + 0.0671575d*E (JD2439320 - 340)
[5683]; since JD2440440 - see
Table.
FurtHer period
increase is possible [9380]. According to [7985]
tHere are two simultaneous oscillations with the
periods P1 and P2: P1 = 0.0654d, P2 = 0.0513d.
P2/P1 = 0.784; A2(U) = 0.25 A1(U).
AE Mic In the interval JD2436670 - 840 Max =
= 2436728.470 + 0.324142d*E. Since JD
2442630 - see Table.
AH Mic Min II 13.6.
AT Mic VB (A 10.83m V, M 4.5Ve; B 10.9m V, M 4.5Ve; a =
= 6.40", P = 675 yr, e = 0.60 [9381]. mu alfa = + 0.0216s, mu delta =
= - 0.331" (mu, Vr, pi - common with AU Mic).
Unusually high freguency of flares
allows to suppose that both components are variable.
The range of combined brightness variation of the
system is given in the Table.
AU Mic mu alfa = +0.0212S, mu delta = -0.348" (mu, pi, Vr - com -
mon with AT Mic).
SB? 0.20P <= M - m <= 0.55P.
THere are periodical light variations and
also flares with A <= 0.5m U [8601].
AW Mic mu alfa = +0.0077s, mu delta = -0.089".
Shape of the light curve strongly varies. Multiperio-
dicity is possible.
AX Mic mu alfa = -0.2805s, mu delta = -1.152". In
minimum brightness B - V = +1.42, U - B = +1.20.
R Mon Peculiar non-stel-
lar object at the apex of the reflection variable [9396]
cometary nebula NGC 2261. Probably young star sur-
rounded by dust cloud. Light curve in [9394].
S Mon In the open star cluster
NGC 2264. VB A (B 8.2m, 2.9", 213deg; 9.9m, 16.6", 14deg.)
T Mon SB (Porb> = 70 yr [9397]). [A/H] = 0.3.
THere is a sguare term in the elements given in the
Table: +5.34d*10**-6*E2.
Deviations from the parabola in the O - C, E diagram
have a wave-like trend. If this wave is attributed to
the light-time effect, Porb = 100 years.
The observations
are also satisfied by the following system of linear
elements: Max = 2412874.56 + 27.0093d*E (JD
2405200 - 15250) [9398]; Max = 2426004.62 + 27.0180d*E
(JD2415250 - 27150); since JD2427150 -
Max = 2436137.090 + 27.0205d*E [2392].
U Mon P var. Min = 2408897 + 92.26d*E (JD2408800 -
36210) [0368]; since JD2437300 -
see Table.
Mean mag-
nitude varies with the period 2320d [0657]. Spectrum
investigation [2226].
V Mon P var. Max = 2412172 + 334.5d*E (JD2412000 -
23500) [0458]; Max = 2427870 + 332.5d*E (JD2423500 -
28200); Max = 2429904 + 342.0d*E (JD2428200 -
30800); Max = 2439570 + 331.6d*E (JD2430800 -
41225); since JD2441225 - see
Table.
X Mon P var. Max = 2415078 + 154.0d*E (JD2415000 -
18800); Max = 2419758 + 149.6d*E (JD2419700 -
21000); Max = 2421136 + 155.0d*E (JD2421000 -
24600); Max = 2424673 + 169d*E (JD2424600 -
25600); Max = 2425644 + 155.6d*E (JD2425600 -
26800); Max = 2427028 + 150.7d*E (JD2427000 -
28000) [0458]; Max = 2429521 + 155.8d*E (JD
2428000 - 36300); Max = 2438846 + 145.3d*E (JD
2437800 - 38900); since JD2440800 -
see Table.
The amplitude
strongly varies; sometimes irregular light variations
are observed.
Y Mon P var. Max = 2415792 + 228.6d*E (JD2415300 -
19700); Max = 2419928 + 227.4d*E (JD2419700 -
24300) [0458]; Max = 2432647 + 233.3d*E (JD
2424300 - 32900); since JD2432900 -
see Table.
RR Mon P var. Max = 2417476 + 384.5d*E (JD2417400 -
19600) [0458]; since JD2419600 -
see Table.
RU Mon Min II 11.06; D II var: 0.06P <= DII <= 0.12P; Min II - Min I
var: 0.25P < = Min II - Min I <= 0.75P. P var.
In the interval JD2429100 - 38409 Min I =
= 2418357.0140; 3.5846794d(E - 406) - 0.429d cos alfa +
+ 0.06d sin 2alfa + 0.010d cos 3alfa + 0.003d sin 4alfa, MinII =
= 2418355.2220 + 3.5846794d(E - 406) + 0.429d cos alfa +
+ 0.060D sin 2alfa - 0.010d cos 3alfa + 0.003d sin 4alfa (JD
2416900 - 29100); Min I = 2429641.567 + 3.5846391d*
(E - 3554) - 0.429d cos alfa + 0.060d sin 2alfa + 0.010d*
*cos 3alfa + 0.003d sin 4alfa, Min II = 2429639.775 +
+ 3.5846391d(E - 3554) + 0.429d cos alfa + 0.060d sin 2alfa -
- 0.010d cos 3alfa + 0.003d sin 4alfa, where alfa =
= 0.01245deg(E - 406) [3445].
The epochs E are being calculated for
Min I from JD hel. 2416901.205, and for Min II -
from JD hel. 2416900.248.
In the interval JD2438409 - 41743
Min I = 2438409.6045 + 3.584586d(E - 6000) - 0.4290d*
*cos alfa + 0.0620d sin 2alfa + 0.0107d cos 3alfa + 0.0026d*
*sin 4alfa - 0.00036d cos 5alfa, Min II = 2438407.8122 +
+ 3.584586d(E - 6000) + 0.4290d cos alfa + 0.0620d sin 2alfa -
- 0.0107d cos 3alfa + 0.0026d sin 4alfa + 0.00036d cos 5alfa,
where alfa = 0.012385deg(E - 406) [7987].
since JD2441743 - Min I = 2441743.2633 +
+ 3.584670d(E - 6930) - 0.4336d cos alfa + 0.0634d sin 2alfa +
+ 0.0111d cos 3alfa + 0.0021d sin 4alfa, Min II =
= 2441741.4710 + 3.584689d(E - 6930) + 0.4336d cos alfa +
+ 0.0634d sin 2alfa - 0.0111d cos 3alfa + 0.0021d sin 4alfa,
wHere alfa = 70.6deg + 0.0114deg(E - 6094) [9546].
Linear elements for Min I epochs in 1973 -
1990 are given in the Table. Corresponding elements
for Min II epochs are: Min II = 2441741.575 +
+ 3.584567d*E. E = 0.38.
Apsidal motion period is 285 years.
RV Mon Mean brightness varies with P = 1047d.
RW Mon Min II 9.45; d I = 0.027P, d II = 0.023P. P var. Min I =
= 2417943.687 + 1.9061012d*E (JD2417940 - 32900)
[3450]; since JD2432900 - see
Table.
RX Mon P var. Max = 2418980 + 343.2d*E (JD2416200 -
19000); Max = 2423097 + 338.9d*E (JD2422000 -
28500); since JD2428500 - see
Table.
RY Mon VB A (B 12.29M, 28").
SS Mon In the region of
the open cluster NGC 2264.
SU Mon S 5/7 - S 6/7. P var: 69d (JD2416700 - 19100); 203.5d
(JD2420100 - 22920); 69d (JD2423000 - 30100).
In the intervals JD2423000 - 520 -
const (11.5m), JD2424820 - 980 - const (11.8m).
SV Mon [A/H] = 0.2. P var. Max = 2419041.805 + 15.230721d*E
(JD2412000 - 22000) [0025]; Max = 2422651.931 +
+ 15.23256d*E (JD2422600 - 23850) [9400]; Max =
= 2424571.60 + 15.2513d*E (JD2423850 - 24600);
Max = 2434045.326 + 15.2304d*E (JD2424600 - 34100);
since JD2433000 - see Table.
SX Mon Mean bright-
ness varies with P = 1100d.
SZ Mon VB A (B 11m - 12m, 10" [9401]). Min II 10.55. P var.
Min I = 2426357.1 + 32.760d*E (JD2422000 - 26400);
Min I = 2427861.2 + 32.708d*E (JD2426750 - 32000);
since JD2432800 - see Table.
Shape of the
light curve varies. Heights of maxima and depths of
minima are constant.
TU Mon Min II 9.1.
TV Mon In the region of
the open star cluster NGC 2237.
TW Mon Wachmann [3453] assigns the variable to the RRab
type with the elements Max = 2433001.371 +
+ 0.8743887*E, but notes a considerable dispersion
of the points around the mean light curve obtained
with this period. As the periods by Hessner (PH)
and Wachmann (PW) are mutually related (1/PW ~
~ 1/PH + 1) it is more probable on account of the
above mentioned circumstance that the variable be-
longs to cepheids.
TX Mon [A/H] = -0.3.
UV Mon The form of
the light curve being unusual for RR Lyr type va-
riables (Max II 13.5 at the phase 0.39P, Min II 13.8
at the phase 0.22P), the period may be doubtful,
though it was found independently by two investiga-
tors [0380, 3453].
UX Mon Min II 8.52; dI = 0.044P. P var?
Brightness in ma-
ximum varies with the amplitude up to 0.2m.
VV Mon Min II 9.55; dI = dII = 0.07P.
There is
a square term in the elements given in the Table:
- 0.12d*10**-7*E**2.
VW Mon P var. Max = 2425243.40 + 0.6041350d*E (JD2414700 -
30700); since JD2430700 - see
Table.
In [0386, 5448] And otHer pre -
vious works the spurious period value 1.532d is
being accepted suggesting the curious nature of the
variable. Serious observations are necessary to se -
lect the true value of the period.
VX Mon Depth of Min II 0.07m.
VY Mon In the region of the nebula
IC 446.
XX Mon [A/H] = -0.2.
XZ Mon Min II 13.6; d = 0.02P:.
AA Mon [A/H] = -0.9. P var. Max = 2430788.266 + 3.938052d*E
(JD2425300 - 34800) [3453]; since JD
2434800 - see Table.
AC Mon In the region of
the open cluster NGC 2323.
AK Mon P var. Max = 2425279 + 319.2d*E (JD2425200 -
28000); since JD2428000 - see
Table.
AN Mon Min II 11.7:; d = 0.027P.
AO Mon Min II 10.16; DII = 0.14P; Min II - Min I = 0.4933P. P var.
Min I = 2426735.333 + 1.884758d*E (JD2426700 -
40000); since JD2440000 - see
Table.
AQ Mon Min II 10.9; DII = 0.05P; dI = 0.014P.
AR Mon Min II 9.03; d = 0.011P.
There is
a square term in the elements given in the Table:
- 1.22d*10**-6*E**2.
AU Mon Min II 8.2:. Shape
of the light curve varies.
Brightness in maximum varies perio-
dically with the amplitude 0.2m: Max = 2443105 +
+ 411d*E; M - m = 0.5P.
AV Mon Depth of Min II 0.04m.
AW Mon P var. Min = 2425649.053 + 20.797d*E (JD2425500 -
26400) [9408]; Min = 2426439.340 + 20.81905d*E (JD
2426400 - 35900) [0511]; since JD2435900 -
see Table.
AX Mon Bina-
ry system with an envelope and gaseous streams.
Porb = 232.60d [6103]. Spectrum investigation [9411].
Epoch of Min brightness preceeding the moment of
conjunction for 0.25p is given in the Table; A = 0.4m U.
Besides periodical variations, there are rapid light
fluctuations up to 0.1m.
BB Mon See AV Mon.
BC Mon P var. Max = 2421240 + 275.8d*E (JD2421200 -
25960); Max = 2428880 + 267.2d*E (JD2425960 -
30000); since JD2430000 - see
Table.
BE Mon delta(S) = 0.
BH Mon d = 0.01p:.
BM Mon Min II 12.3. According to [9415], apsidal motion is
possible.
BO Mon Min II 10.1. P var. Min I = 2428211.596 + 2.2251753d*E
(JD2415000 - 36000) [0007]; since JD
2436000 - see Table.
BP Mon P var?
Elements given
in the Table are valid in the interval JD2425600 -
29700.
BT Mon VB A (B 16.0m, 10", 0deg).
After the outburst in 1939 the brightness va-
ries in the range 16.0m - 18.7m with the elements: Min =
= 2443491.7155 + 0.3338141d*E; D = 0.20p, 0 <= d < = 0.03p.
Before the out-
burst in 1939, according to [9417], the following ele -
ments were valid: Min = 2429500.207 + 0.3338010d*E.
Emission nebula with
the radius of 3.8" was discovered in 1981 around
the nova [9148].
BX Mon Usually was considered as mira type variable
[9421]. In the Table the epoch of light maximum and
the period are given according to [9419]. According
to [9420] the Balmer emission lines originate in the
nebulosity surrounding the symbiotic system and are
excited by the hot component, and light variations
are due to the orbital motion in the system.
BZ Mon d = 0.030P. In the
region of the open cluster CR 106.
CC Mon In the region of
the open cluster CR 106.
CD Mon P var. Max = 2427704 + 273.8d*E (JD2427400 -
30400); since JD2430400 - see
Table.
CE Mon Min II 14.2.
CF Mon Min II 13.7; d = 0.02P:.
CH Mon d = 0.030P.
CS Mon VB A (B 13m, 9", 0deg).
CT Mon In the region
of the open cluster NGC 2244.
CU Mon [A/H] = -0.2.
CV Mon In
the centre of an anonymous open cluster.
VB A (B 13.76m, 10", 270deg; C 13.72m, 14", 270deg).
P var. Max = 2429805.142 + 5.378782d*E (JD2429360 -
36000); since JD2436000 - see
Table.
DD Mon Min II 11.3.
DF Mon The chart in [5285] is wrong, the star observed was
not DF Mon.
DN Mon Min II 13.9.
DR Mon See CC Mon.
DT Mon P var. Max = 2425324 + 345d*E (JD2425300 - 28200)
In the interval JD2429250 -
37700 tHere were cycles 119d,
230d, 350d.
DW Mon In the region
of the open cluster NGC 2286.
EE Mon P var. Max = 2425300.42 + 4.80776d*E (JD2425300 -
27720); since JD2427720 - see
Table.
EH Mon d = 0.023P.
EK Mon P var. Max = 2425302.59 + 3.95773d*E (JD2425200 -
33000) [0387]; since JD2433000 -
See Table.
EP Mon d = 0.026P.
ES Mon d = 0.02P.
EW Mon Min II 14.2.
FH Mon See AV Mon.
FP Mon In the region of
the open cluster NGC 2353.
FS Mon Min II 11.2.
FU Mon S 6.5/7.5.
FW Mon d = 0.016P. See AV Mon.
FX Mon OH emission.
FZ Mon The elements
should be checked.
GH Mon Min II 13.1.
GP Mon See SS Mon.
GQ Mon See SS Mon.
GR Mon See SS Mon.
GU Mon Min II 12.5.
GV Mon See AV Mon.
GX Mon OH, H2O, SIO maser.
HI Mon Min II 9.9.
HM Mon Min II 13.6. P var. Min I = 2430110.1948 + 0.40765737d*E
(JD2429600 - 35400) [5285]; since JD
2435400 - see Table.
HO Mon d = 0.03P.
HP Mon d = 0.04P:.
HR Mon Depth of Min II 0.03m.
HY Mon Min II 12.4.
IL Mon d = 0.03P.
IM Mon Min II 6.47.
IO - IQ Mon
See SS Mon.
IR Mon P var?
IS Mon Depth of Min II 0.05m.
IX Mon Min II 12.8.
IZ Mon Min II 12.0.
KU - MN Mon
See SS Mon.
MO Mon VB A (B 20m, 10", 356deg); see SS Mon.
MP - MQ Mon
See SS Mon.
MX Mon Min II 11.7.
NN Mon Min II 12.9.
NS Mon Min II 11.1.
NT - OW Mon
See SS Mon.
OX Mon VB A (B 15m, 7", 35deg); see SS Mon.
OY - PQ Mon
See SS Mon.
PR Mon See FZ Mon.
PT - PY Mon
See SS Mon.
QR Mon 290d <= P <= 400d.
Depth of Min varies by
0.9m with the period about 2000d.
QT- V346 Mon
See SS Mon.
V347 Mon VB A (B 20m, 12", 120deg); see SS Mon.
V348- V355 Mon
See SS Mon.
V356 Mon VB (3", 78deg); see SS Mon.
V357- V364 Mon
See SS Mon.
V365 Mon VB B (A = V591 Mon, B 7", 135deg); see SS Mon.
V366- V367 Mon
See SS Mon.
V368 Mon VB (9", 252deg); see SS Mon.
V369 Mon VB (11", 264deg); see SS Mon.
V370 Mon VB (8", 97deg); see SS Mon.
V371 Mon See SS Mon.
V372 Mon SC 7/7.5.
V373 Mon See SS Mon.
V379 Mon d = 0.015P:.
V380 Mon Min II 12.9; P = 1.98904166d?
V383 Mon Min II 15.2.
V384 Mon Min II 13.0.
V389 Mon Min II 14.9.
V393 Mon Min II 14.3.
V394 Mon d = 0.02P; see AV Mon.
V395 Mon d = 0.03P.
V396 Mon Min II 13.5.
V397 Mon Min II 11.9.
V398 - V403 Mon
See SS Mon.
V404 Mon d = 0.02P:.
V405 - V425 Mon
See SS Mon.
V426 Mon VB A (B = NSV 3125 17.0m, 6", 117deg); see
SS Mon.
V427 - V441 Mon
See SS Mon.
V442 Mon Min II 11.6.
V443 - V444 Mon
See SS Mon.
V445 Mon Min II 11.3.
V446 Mon [A/H] = -0.7.
V447 Mon [A/H] = -1.4.
V448 Mon Min II 9.8.
V449 Mon d = 0.02P.
V450 Mon Min II 12.6.
V451 Mon Min II 14.7.
V452 Mon Min II 12.7; d = 0.02P.
V453 Mon Min II 11.8.
V454 Mon Min II 12.2.
V455 Mon Min II 15.3.
V456 Mon Min II 13.7.
V457 Mon Min II 14.3; d = 0.03P:.
V458 Mon Min II 13.8.
V459 Mon Min II 14.7.
V460 Mon Min II 10.7.
V463 Mon d = 0.03P; P = 2.2476768d?
V464 Mon Min II 12.3.
V465 Mon P var. Max = 2429642.44 + 2.71341d*E (JD2425600 -
30800) [3551]; Max = 2431845.65 + 2.713212d*E (JD
2430000 - 35200) [3453]; Max = 2435541.315 +
+ 2.713668d*E (JD2435200 - 41600); since
JD2441600 - see Table.
V466 Mon VB A (B 15m, 135deg).
V474 Mon (k - b)2 = 0.32. Blazhko effect:
Max(O - C) = 2441664.962 + 7.74639d*N; Min(O - C) =
= 2441669.569 + 7.74639d*N; 0.03m <= A <= 0.37m; - 0.02d <=
<= O - C <= + 0.03d.
Freguency analysis gives three prin-
cipal oscillations [8669]: P1 = 0.1361258d (A1 = 0.18m),
P2 = 0.1337745d (A2 = 0.12m), P3 = 0.1385591d (A3 =
= 0.04m).
V478- V479 Mon
In the region of the
nebula IC 2169.
V481- V483 Mon
See V478 Mon.
V486 Mon VB A (B 18.4M, 6"). See V487 Mon.
V487- V489 Mon
In the region of the
nebula NGC 2245.
V490 Mon In the region of the nebula
NGC 2247.
V493 Mon In the region of
the open cluster Tr 5.
V494 Mon See IS Mon.
V496 Mon Min II 12.8.
V497 Mon 8.9 - 11.8 IR.
V498 Mon P = 2.4727818d?
V500 Mon See SS Mon.
V501 Mon Min II 13.1; Min II - Min I = 0.445P; DII = 0.036P.
V503 Mon 9.2 - 10.9 IR.
V505 Mon Min II 7.55.
V507 Mon SB2 (P = 53.781d [9483]); d = 0.015P:.
V510 Mon [A/H] = - 0.1.
V513 Mon See AV Mon.
V514 Mon Min II 13.3.
V515 Mon Min II 12.7.
V521 Mon Min II 10.4.
V524 Mon Min II 15.2.
V526 Mon P var. Max = 2433304.284 + 2.675208d*E (JD2429300 -
35170); since JD2439170 - see
Table.
V527 Mon See IS Mon.
V530 Mon Min II 12.8.
V532 Mon Min II 12.8. RRC?
V535 Mon P var. Max = 2431846.445 + 0.3328791d*E (JD
2429600 - 34060); since JD2434060 -
see Table.
[Fe/H] = - 1.44.
V539 Mon See CT Mon.
V540- V542 Mon
See VY Mon.
V543- V549 Mon
See CT Mon.
V550 Mon VB A (B 17.3m, 6", 0deg ); see CT Mon.
V551- V557 Mon
See CT Mon.
V560 Mon See IS Mon.
V565 Mon Connected with the diffuse nebula
NGC 2313 having diameter of 10" and a faint come-
tary nebula.
V569 Mon VB A (B 10.8m, 6.2", 281deg; C 10.5m, 38.3", 295deg).
The range of combined light varia-
tion of A and B components is given.
According to [8215], P = 0.18d.
V571 Mon (k - b)2 = 0.32.
Non-radial pulsation with va-
riable periods: P1 = 0.0999081d (A1 = 0.052m), P2 =
= 0.0749998d (A2 = 0.015m) (JD2440914 - 41692)
[7127]; P1 = 0.0894534d (A1 = 0.038m), P2 = 0.15988d
(A2 = 0.025m), P3 = 0.106516d (A3 = 0.014m). P4 = 0.26998d
(A4 = 0.012m), P5 = 0.15069d (A5 = 0.011m) (JD
2441662 - 719) [9450].
V577 Mon VB (A 11.3m V, B 14.8m V; a = 0.312", P = 16.60 yr, e =
= 0.38); mu alfa = + 0.049S, mu beta = + 0.73".
Both components are probably variables. The range
of combined light variation of the system is given
in the Table [6146].
V578 Mon See CT Mon.
V579 - V586 Mon
See SS Mon.
V588 - V589 Mon
See SS Mon.
V590 Mon VB (10", 358deg); see SS Mon.
V591 Mon VB A (B = V365 Mon, 7", 135deg); see SS Mon.
V593 - V612 Mon
See SS Mon.
V613 Mon S 3/2.
V616 Mon Novalike outbursts were ob-
served in 1917 (Max JD2421540) and in 1975 (Max
JD2442646). In quiescent state probably ellipsoi-
dal light variation is observed with P = 0.325d and
A = 0.2m [9458], and also slower light variations
with P = 7.39d [9459] or 7.8d [9460]. Spectrum descrip-
tion [9461, 9462].
V624 Mon See CC Mon.
V628 - V629 Mon
See SS Mon.
V630 Mon VB A (B 21m, 3", 300deg); see SS Mon.
V632 Mon In the region of
the open cluster NGC 2368.
V637 Mon Basic oscillation
with A1 = 0.05m and elements given in the Table is
superimposed by the second one with A2 = 0.02m and
the elements: Max = 2443496.1624 + 0.19740d*E.
Beat period Pb = 6.09d.
V638 Mon VB (6.5m, 8.5m; 0.8", 178deg).
V640 Mon See CT Mon. Porb = 14.39604d [6103].
Irregular light variations.
Probably transitional stage from a binary system of
O stars to a system of WR type [4107].
V641 Mon VB A (B 10.91m, 21.4", 310deg; C 12.46m, 25.8", 285deg).
See SS Mon. Depth of Min II
0.07m.
V642 Mon See SS Mon. Cluster non-
member. Epoch of light
minimum is given in the Table.
V645 Mon Epoch of light minimum
is given in the Table.
S Mus Marked on the
chart for BO Mus. Max II = Max I, ” (Max II) = 0.15P.
P var? SB 1 (Porb = 506.4d).
T Mus P2 = 1021d.
V Mus In the coal sack
region.
RV Mus P = 128d: is possible.
RW Mus P = 130d: is possible.
RY Mus V1 (NGC 4833).
RZ Mus V2 (NGC 4833). Cluster non-
member.
SY Mus Min II 11.2; Min I - Min II = 170d.
Elements for Min I of quasiperio-
dic variations observed during JD2434910 - 41510
are given. Radio source.
TU Mus Min II 8.65. P var. Min I = 2424260.396 + 1.38728d*E
(JD2423900 - 29300) [0039]; during
JD2437380 - 41900 - see Table.
The light curve shape var.
TV Mus Min II 11.3.
TW Mus Min II 12.4.
TZ Mus B - V: +1.22, +1.43.
UW Mus Min II 11.9.
UY Mus Min II 12.0.
VW Mus Min II 13.9.
WY Mus P var. Periodic term:
+ 0.35d*sin (0.12deg*E).
XZ Mus Before JD2419200 Max = 2412590 + 113d*E.
AB Mus Min II 13.0.
AS Mus [A/H] = 0.5.
AX Mus P var. During JD2412550 - 19200 -
see Table; during JD
2423900 - 26100 P = 97.3d.
AY Mus Min II 10.8. Min II - Min I = 0.481P.
The elements are valid during 1897 -
1943. In the time interval JD2441683 - 721 ec-
lipses did not occur [8094].
BB Mus P, possibly P should
be doubled.
BD Mus Depth of Min II 0.05m.
BE Mus Min II 14.1.
BF Mus Min II 14.4.
BK Mus P very long P: 56d < d < 310d.
BR Mus Min II 11.25. B - V: +0.10m.
BS Mus Min II 11.5.
BX Mus Depth of Min II 0.04m.
CD Mus Min II 14.7.
CS Mus P > 120d.
DW Mus According to
[8135], the spectral type is M5e, typical of Mira
stars. Elements in [3934] were deduced from the ob -
served brightness variations with P ~ 355d which
was considered to be a spurious period; rapid varia -
tions were confirmed by 7h of photographic obser -
vations.
DZ Mus See BB Mus.
EE Mus In the coal sack. The flare was observed
spectroscopically.
EN Mus d = 0.035P:.
EP Mus [A/H] = 0.2. According to [8136], EA,
P = 4.15d, D = 0.05P, 11.63m - 12.60m V, Min II 11.7:.
ET Mus Alternatively possible type
EW [8727, 4001].
EV Mus d = 0.09P:.
EY Mus See V Mus.
EZ Mus Alternative possible
values of P 4.3032d, 4.3224d.
FH Mus Depth of Min II 0.03m.
FO Mus P var?
GK Mus Min II 15.0.
GN Mus Min II 14.2.
GO Mus Min II 15.2.
GP Mus B - V: +1.03, +1.61.
alf Mus VB A (B 13.0m, 29.3", 316deg).
eta Mus VB A (B 7.30m, 60").
tet Mus VB (A 5.64m, B 7.5m, 5.3", 187deg); SB (Porb = 18.341B).
Variable intensity of emission
lines with respect to the continuum (double wave;
elements in the Table are for the epochs of Min I
variability in the UV range (lambda lambda 1550 - 3300 A) with
an amplitude about 2%, P = 1.5d And rapid changes
(lamda lamda 1550 - 1800 A) with an amplitude about 3 - 5% ON
the time scale of 50s - 70s [8532].
Connected with a nebula,
80'*45'.
R Nor VB A (B 14.0m, 5.7", 268deg, 1929). P var. Max II =
= 2406371 + 486.94d*E (JD2406300 - 25000); Max II =
= 2426359 + 500.56d*E (JD2426000 - 30500); Max II =
= 2431377 + 489.0d*E (JD2430500 - 34500);
since JD2437600 - see Table.
Like R Cen, has a doudle Max,
divided by a comparatively shallow Min II. Max II is
usually brighter than Max I. ” (Min I) = 0.43P,
” (Max I) = 0.70P, ”(Min II) = 0.85P.
S Nor In the centre of the open cluster
NGS 6087, cluster member.
[A/H] = -0.1.
T Nor P var.Max = 2414783 + 241.87d*E (JD2414700 -
28000); Max = 2428084 + 244.93d*E (JD2428000 -
35000); since JD2437000 - see
Table.
U Nor P var. Max = 2415028.94 + 12.64084d*E (JD2415000 -
26000) [0060]; since JD2434000 -
See Table, [A/H] = -0.6.
W Nor P2 ~ 1300d.
Y Nor VB A (B 12.2m vis, 4.0", 156deg, 1903).
Z Nor Min II 9.6.
RR Nor Min II 9.9.
RS Nor B - V: +1.13, +1.48.
RT Nor Quasiperiodic varia-
tions: P1 ~ 59d, P2 ~ 175d [8140].
RV Nor [A/H] = 0.8.
There are irregularities in the light curve.
SV Nor Min II 12.6.
SW Nor d = 0.003P.
SX Nor d = 0.1P.
SY Nor VB A (B 12.8m, 2.1", 315deg, 1934). B - V: +1.16, +1.49.
[A/H] = 0.5.
SZ Nor Min II 12.6.
TT Nor Twice longer P is
possible.
TU Nor Min II 12.5.
Associated with a small faint nebula.
TV Nor Min II 9.3.
TW Nor In the
region of the poor open cluster Lynga 6. B - V: +1.79,
+2.22. [A/H] = 0.2.
TX Nor Min II 12.5.
TZ Nor Min II 12.1.
UV Nor d ~ 0.07P.
UX Nor In Max light B - V = +0.30.
UY Nor d = 0.025P.
UZ Nor d = 0.02P.
VV Nor In the region of the cluster
NGC 6152.
VX Nor Depth of Min II ~ 0.03m.
VZ Nor See VV Nor.Min II 14.3.
WX Nor The chart is erroneously labelled as that
for WZ Nor. Min II 12.8.
WZ Nor The chart is erroneously labelled as that
For WX Nor. Min II 13.4.
XY Nor Min II 13.2.
AA Nor [A/H] = -0.1.
AF Nor In the region of
the open cluster NGC 5999.
AT Nor d = 0.026P:.
BE Nor Min II 14.2.
BH Nor Min II 13.2.
BP Nor Close companion.
CE Nor d = 0.05P. Min II 11.8?
CX Nor Min II 15.0.
DO Nor Min II 14.2. See DR Nor.
DR Nor In the region of
the open cluster NGC 6087.
EM Nor Min II 13.8.
ET Nor d = 0.032P.
FK Nor Min II 15.0.
FQ Nor According to [0060], P = 1.994d?
FW Nor Min II 14.5.
GM Nor d = 0.02P; Min II 11.01; Min II - Min I = 0.499P
(JD2441683 - 721), Min II - Min I = 0.531P (JD2425381 -
28402). B - V = 0.44m.
GN Nor Min II 13.3, DII = 0.16P, Min II - Min I = 0.405P
(JD2425900). Apsidal mo-
tion: P = 500yr.
GO Nor Min II 13.7.
GQ Nor Min II 13.8.
GR Nor [A/H] = 0.9.
GT Nor d = 0.048P.
GU Nor See IS Nor. B - V: +1.17, +1.40. [A/H] = 0.1.
GV Nor d = 0.03P:.
GX Nor Min II 15.0.
HH Nor VB B (A 9.9m vis, FO; B 12.6", 148deg). d = 0.05P.
HI Nor D is very small.
HK Nor Min II 12.9.
HO Nor Min II 13.2:.
HW Nor d = 0.024P.
HZ Nor P = 2.921584d is possible.
IQ Nor B - V: +1.55, +1.93.
IS Nor In the region of
the open cluster NGC 6067.
IT Nor Min II 9.8.
KL Nor P >= 140d.
KM Nor P >= 170d.
KQ Nor Mira Ceti type is not
excluded [4001].
KT Nor P >= 180d.
KX Nor Min II 14.8.
LO Nor P >= 220d.
LV Nor Deep Min II.
LX Nor Possible P values:
0.60492d, 0.7851d, etc.
NR Nor Min II 15.9.
NW Nor P > 140d.
NX Nor Min II 14.4.
OS Nor Epoch of
Min is given. EW/KW type is possible.
OT Nor Min II 13.7.
OU Nor Min II 15.1.
OV Nor P >= 200d.
OW Nor P >= 120d.
OX Nor P >= 110d.
PQ Nor Possibly a cepheid which is a fainter compo-
nent of an unresolved binary. Epoch of Max is given.
PT Nor See IS Nor.
QV Nor 3U 1538 - 52. No.12 [4124].
Epoch of Min cor-
responding to the X-ray eclipse is given. Depth
of Min I 0.05m V, that of Min II 0.08m V. The peri-
od of X-ray pulses Px = 528.928s [4114]. A flare
was observed with delta(m) > 0.3m [9456].
OX Nor 4U 1608 - 52.
QZ Nor In the open cluster
NGC 6067.
MU Nor In the regi-
on of the open cluster NGC 6169.
U Oct P var. Max = 2420685 + 302.00d*E (JD2414900 -
20700); Max = 2424320 + 300.74d*E (JD2422800 -
29800); Max = 2431901 + 309.60d*E (JD2429800 -
32250); Max = 2434018 + 300.70d*E (JD2432250 -
38800); since JD2438800 -
See Table.
X Oct P var.Max = 2415170 + 208.40d*E (JD2415100 -
17100); Max = 2417425 + 201.24d*E (JD2417100 -
20700); Max = 2423780 + 207.95d*E (JD2422000 -
24000); Max = 2424370 + 200.18d*E (JD2424000 -
25600); since JD2425600 -
see Table.
Depths of minima ape stongly variable;
1.1m <= A <= 4.0m.
RV Oct delta(S) = 10.
TX Oct Min II 12.7.
UV Oct delta(S) = 9; (k - b)2 = 0.06. Blazhko
effect: P = 80d; 0.14P <= M - m <= 0.24P, 0.4m <= A <= 1.3m.
UZ Oct Min II 9.48; dI = 0.00P, dII = 0.05P. P var. Min I =
= 2440223.1560 + 1.1493709d*E (JD2438300 -
42000); since JD2442000 -
See Table.
AM Oct Min II 14.9.
BE Oct P < 20d:.
BG Oct P = 0.7490d?
BK Oct Min II 14.6.
BP Oct (k - b)2 = 0.25.
CC Oct Basic radial pulsation with P1 = 0.12490d (A1 = 0.042m)
is superimposed by otHers with periods: P2 = 0.0795317d
(A2 = 0.008m), P3 = 0.12336d (A3 = 0.014m); P4 =
= 0.11068d (A4 = 0.008m), P5 = 0.12713d (A5 = 0.006m);
P6 = 0.11815d (A6 = 0.006m).
CD Oct mu = 0.51", p = 279deg. One of the pe-
riods P = 686s (A = 0.01m).
CE Oct Light oscillation
with P2 = 0.054511d (A2 = 0.0056m) is superimposed
by an oscillation with P1 = 0.2100d or 0.2660d (A1 =
= 0.0052m), which is due to pulsation or ellipsoidal
variability in a close binary system.
R Oph P var. Max = 2399214 + 302.1d*E (JD2399200 - 2427900)
[0458]; Max = 2427915 + 304.0d*E (JD2427900 - 34900);
Max = 2434906 + 301.5d*E (JD2434900 - 40600) [0001];
since JD2440600 - see Table.
U Oph ADS 10428 A (B 12.26m, GOV, 20.4", 358deg). Min II 6.46.
P var. Periodic term: + 0.0120d*
*sin (0.0483deg*E + 4.7833deg).
V Oph P var. Max = 2411155 + 296.73d*E (JD2411000 - 24000);
Max = 2424198 + 302.46d*E (JD2424000 - 28000);
since JD2428000 - see Table.
W Oph P var. Before JD2420500 Max = 2415186 +
+ 335.07d*E; Max = 2420870 + 325.33d*E (JD2420500 -
24700); since JD2424700 - see
Table.
X Oph VBA (A = 0.34", Porb = 485.3 yr; B - 9m, K1III, 0.4", 142deg,
1980).
The range of the combined brightness is given.
P var. Max = 2416416 + 336.61d*E (JD2416400 - 26000);
Max = 2426161 + 331.28d*E (JD2426000 - 32500); Max =
= 2432788 + 335.50d*E (JD2432500 - 38000);
since JD2438000 - see Table.
Y Oph SB1? Porb = 2612d? P var. Before JD2427000
Max = 2408694.77 + 17.11884d*E; since
JD2432000 - see Table. [A/H] = -0.2.
Z Oph P var. Max = 2411896 + 349.0d*E (JD2411800 - 21000)
[0458]; Max = 2420962 + 352.1d*E (JD2421000 - 25000);
Max = 2425183 + 347.4d*E (JD2425000 - 31000);
Mean elements after JD2431000 -
see Table.
RR Oph P var. Nonlinear term:
- 0.009282d*E2.
RS Oph Previous outbursts: 1898,
1933, 1958.
According to [7575], in
1972 - 1973 tHere were semiregular variations (delta(m) ~
0.5M, P = 50D - 70D).
RT Oph P var. Before JD2426500 Max = 2417452 +
+ 429.00d*E; Max = 2426461 + 422.67d*E (JD2426500 -
34000); since JD2434500 - see
Table. OH, H2O maser.
RU Oph P var. Before JD2422000 Max = 2417388 +
+ 200.95d*E; Max = 2422011 + 203.62d*E (JD2422000 -
27300); Max = 2427298 + 200.5d*E (JD2427300 - 29000);
Max = 2429305 + 203.88d*E (JD2429000 - 33000);
during JD2433000 - 40500 - see
Table.
RV Oph d = 0.015P; Min II 9.56, DII = 0.09P.
The light curve share var.
RW Oph P var. Max = 242494 + 247.86d*E (JD2425000 - 34000).
The Table gives
mean elements.
RX Oph OH, H2O maser.
RY Oph P var. Max = 2415235 + 151.05d*E (JD2414700 - 24000);
Max = 2424152 + 149.69d*E (JD2424000 - 31000); Max =
= 2431339 + 150.94d*E (JD2431000 - 40000);
since JD2440000 - see Table.
RZ Oph d = 0.030P.
SS Oph P var. Before JD 2432500 Max = 2417330 +
+ 179.88d*E.
ST Oph (k - b)2 = 0.03.
SV Oph The elements are valid
since JD 2422000.
SW Oph VB A (B 12.0m vis, 2.4", 91deg, 1943). d = 0.02P. P var.
Min = 2418880.528 + 2.445948d*E (JD 2418880 - 26200)
[0001]; Min = 2431235.216 + 2.446086d*E (JD 2427900 -
33500) [2389]; since JD 2434000 -
See Table.
SX Oph d = 0.03P.
SZ Oph P var. Before JD 2428400 Min = 2421057.556 +
+ 3.708454d*E; since JD 2442000 -
see Table.
TT Oph [Fe/H] = -0.5.
TW Oph P2 = 2000d:.
Associated with a nebula of variable bright-
ness [3479].
UU Oph d = 0.024P. P var?
UX Oph P var. Max = 2426041 + 117.34d (JD 2406430 - 28040);
since JD 2433100 - see Table.
VW Oph P var. Mean elements are
given. During JD 2422500 - 30600
Max = 2430554 + 282.69d*E.
WW Oph Epoch of Min is given.
WZ Oph Min II 9.82.
XX Oph A symbiotic object featuring deep fadings
of long duration [9489].
AH Oph H2O maser.
BF Oph SB? P var? since JD 2430000 -
See Table.
BN Oph 80d <= P <= 250d.
DM Oph P var. P = 220d (1893 - 1910), P = 216d (1914 - 1928).
DQ Oph P = 35d is possible.
FK Oph V2 (NGC 6273).
GM Oph V12 (NGC 6284).
GR Oph P var. Max = 2415425 + 136d*E (1893 - 1908);
during 1910 - 1928 - see Table.
IL Oph P2 = 140d:.
IW Oph In the field of the globular
cluster NGC 6293, possible cluster member.
KM Oph In the field of the globular cluster NGC 6304,
field star.
KO Oph In a dark nebula.
KQ Oph P2 = 1500d.
KR Oph P2 > 5000d.
OU Oph V70 (NGC 6266).
PU Oph VB (A = V29 (NGC 6266), the data
are in the Table; B = V28 (NGC 6266), 16.6m - 17m, 4B,
4.8", 7deg), B: RRAB, Max = 2433423.52 + 0.49749d*E,
M - m = 0.15P.
V378 Oph Min II 14.2.
In the region of the open
cluster CR 359. Epoch of Max is given.
V380 Oph Porb = 0.16d. Blue.
V391 Oph See V 423 Oph. P var? Before JD 2427000
Min = 2425501.425 + 2.89558d*E [0432]; since
JD 2441500 - see Table.
V392 Oph Red.
V402 Oph P var. Max = 2425364 + 154d*E (JD 2425350 - 670);
since JD 2425670 - see Table.
V413 Oph delta(S) = 3. Blazhko effect?
V414 Oph B - V: +0.41, +0.77.
V423 Oph In the region of
the open cluster CR 359.
V426 Oph Outbursts separated by 17d - 55d [8079]; in 1976 - 77 the
cycle was 32.3d. Outside outbursts 12.7m - 13.3m, wa -
ves with a cycle of 20 - 30 Min and slower variations.
V438 Oph H20 Maser.
V439 Oph B - V: +0.63, +0.97.
V442 Oph Porb = 0.14056d.
V445 Oph VB A (B 13.04m y, 21"nf). (k - b)2 = 0.35; delta(S) = 2.
According to [5692], Blazh -
ko effect (Pi > 2000d).
V449 Oph P var. Before JD 243900 Min = 2428696.465 +
+ 1.243078d*E; Min = 2442959.607 + 1.243095d*E
(JD 2439000 - 43000); since JD 2443000 -
see Table.
V451 Oph Min II 8.31; Min II - Min I = 0.494P; DII = 0.12P.
V452 Oph delta(S) = 5:.
V455 Oph P var?
The Table gives mean elements
which need confirmation.
V456 Oph Min II 10.5. P var. Before JD 2436100 Min =
= 2428422.341 + 1.015986d*E [0476]; since
JD 2441800 - see Table.
V465 Oph B - V: +0.68, +1.10. P var?
V471 Oph Very red.
V478 Oph B - V: +0.86, +1.33. [A/H] = -0.7.
The elements need confirmati-
on.
V487 Oph D <= 0.14P. See V 423 Oph.
V496 Oph See V 423 Oph.
V501 Oph Min II 11.1.
V502 Oph Min II 8.81. P var. Since JD 2434500 -
see Table.
V506 Oph Min II 12.0. See V 423 Oph.
V508 Oph Min II 10.59.
V509 Oph See V 423 Oph.
V511 Oph Min II 13.7. See V 423 Oph.
V515 Oph Max = 2425600 + 300d*E (JD 2425600 - 26700); P =
= 140d (JD 2426700 - 27300); during
JD 2427300 - 30200 - see Table.
V516 - V517 Oph
In the region
of the globular cluster NGC 6304.
V521 Oph P = 164d (JD 2415000 - 24600); P2 - 4000d.
V526 Oph Min II 13.6.
V527 Oph Min II 14.8.
V532 Oph P >= 6000d.
V533 Oph P >= 80d.
V534 Oph d = 0.03P.
V535 Oph d = 0.025P.
V536 Oph d = 0.04P:.
V537 Oph Min II 12.8.
V540 Oph d = 0.05P; Min II 13.4.
V541 Oph [A/H] = -1.0.
In the region of the
globular cluster NGC 6401; cluster non-member?
V543 Oph Min II 13.6.
V549 Oph Min II 14.0.
V550 Oph Min II 13.0.
V554 Oph [A/H] = -1.1.
V555 Oph Sharp and
flat maxima. Blazhko effect?
V557 Oph Min II 15.7. See V 423 Oph.
V558 Oph B - V: +0.57, +0.68. [Fe/H] = -1.48. Accor-
ding to [9037], P = 0.299d.
V564 Oph [Fe/H] = -1.37. Epoch of Min is
given. P var. Nonlinear term:
+ 0.0073d*(E + 10)**2.
V565 Oph P = 0.3957d is possible.
Photoelectric observations of 1968 contradict
the elements [5746].
V566 Oph dI = 0.048P; Min II 7.89, dII = 0.06P. P var. Before
JD 2440500 Min = 2436744.4200 + 0.40964091d*E
[8287]; since JD 2440500 - see
Table.
V567 Oph (k - b)2 = 0.22; delta(S) = 0. According to [7984],
Max = 2441134.467 + 0.1300729d*E.
V568 Oph Red.
V570 Oph VB A (B 16.3m, 5", 90deg).
V572 Oph See V 423 Oph.
V573 Oph d = 0.034P. See V 423 Oph.
V574 Oph P2 ~ 500d.
V577 Oph Min II 11.9. Min II - Min I = 0.583P. DII = 0.050P. e = 0.22.
V580 Oph VB A (B 15.5m, 0.2').
V585 Oph A long-period variation is superimposed?
V586 Oph See V 423 Oph.
V590 Oph Min II 13.6.
V592 Oph Max = 2427227 + 78d*E (JD 2426100 - 29400);
during JD 2429400 - 30150 - see
Table.
After intervals of irregular variability the peri -
odicity resumes without phase shift.
V605 Oph See WW Oph.
V618 Oph Min II 14.7:.
V636 Oph d = 0.030P.
V683 Oph P var. The light
curve shape varies.
V687 Oph P may be twice longer.
V693 Oph Blazhko effect? [5692].
V695 Oph P var? The light
curve shape varies.
V698 Oph P var? since JD 2442950 - see Table.
V700 Oph B - V: +0.49, +0.50. [Fe/H] = -2.10.
V716 Oph delta(S) = 7.
V720 Oph VI (NGC 6171). Cluster non-
member.
V722 Oph P var. Max = 2437089.456 + 0.6190385d (JD 2419900 -
37100) [7806]; since JD 2436700 -
See Table.
V729 Oph P var. Max = 2437492.766 + 0.4685794d*E (JD 2423500 -
37800) [3560]; since JD 2437400 -
See Table.
V732 Oph Unusual
light curve (sharp Max; primary Min; broad Max; se -
condary Min 15.2).
V734 Oph P var. MAX = 2420636.497 + 0.562489d*E (JD 2420600 -
29100); during JD 2429100 - 37150 -
see Table.
V735 Oph Min II 10.6.
V737 Oph P = 374d is possible.
V767 Oph According to
[0104], waves with delta(m) = 0.3m - 1.4m vis of 50d - 110d
duration; mean brightness var, delta(m) ~ 0.4m in 800d -
- 1000d.
V782 Oph Very red.
V784 Oph B - V: +0.26, +0.56.
The period should be checked.
V786 Oph Red.
V788 Oph See V822 Oph. Pi = 115d.
V799 Oph P = 215d is possible.
V802 Oph Red.
V816 Oph B - V: +0.25, +0.63.
V822 Oph Blazhko effect?
V823 Oph In the region of
the open cluster IC 4665.
V825 Oph See V823 Oph.
V829 Oph See V822 Oph. Pi = 165d.
V832 Oph Red.
V838 Oph P2 ~ 500d is possible.
V839 Oph mu = 0.041", ro = 292deg. Min II 9.38.
V840 Oph VB A (B 12m, 16", 116deg).
V841 Oph Max = 2396146.
V843 Oph SN Kepler. Max 2307193. Gase-
ous remnant.
V844 Oph Min II 14.9.
V845 Oph VB A (B 15.7m).
V847 Oph Min II 13.1.
V848 Oph Min II 13.4.
V851 Oph Max = 2425828 + 95d*E (JD 2425600 - 29700);
during JD2429700 - 34250 -
See Table.
V854 Oph According to [8116], the spectrum
resembles that of a T Tau - type star.
V868 Oph Min II 13.6. See V423 Oph.
V870 Oph See V823 Oph.
V872 Oph P = 0.825d is possible.
V878 Oph Min II 16.5. See V423 Oph.
V911 Oph P2 = 81d, P3 = 114d. P4 > P3?
Standstills up to 100d.
V919 Oph VB A (B sp).
V920 Oph Min II 15.9.
V924 Oph Min II 16.4.
V929 Oph d = 0.050P.
V934 Oph E type is possible.
V936 Oph See V823 Oph.
V938 Oph Min II 15.3. See V423 Oph.
V940 Oph Min II 15.6.
V941 Oph Min II 16.5.
V943 Oph Min II 16.4. See V423 Oph.
V945 Oph Min II 15.1. See V423 Oph.
V947 Oph Min II 14.5. See V423 Oph.
V952 Oph P = 0.954d is possible.
V954 Oph See V423 Oph. Min II 14.9. According
to [3500], const, V = 12.86m, B - V = +1.36m,
V959 Oph P var? Max = 2429785.419 + 0.084857d*E
(JD 2429785 - 845) [2757]; during
JD 2443719 - 732 - see Table;
otHer possible elemente: Max =
= 2443726.469 + 0.07786d*E.
V960 Oph See V423 Oph.
V963 Oph Min II 15.1. See V423 Oph.
V968 Oph [Fe/H] = -1.48. See V423 Oph.
V969 Oph Min II 13.8:. See V423 Oph.
V977 - V978 Oph
In the region
of the globular cluster NGC 6426.
V979 Oph V11 (NGC 6426). Cluster non-
member.
V980 Oph See V977 Oph. P = 0.25740d is possi-
ble.
V983 Oph See V423 Oph.
V986 Oph In July 1980 Vr
varied with P = 0.179d, 0.147d, 0.225d, and possibly
0.097d, but there were no spectrum variations, and
the photometric P = 0.323d was not noticeable in Vr.
SB? Porb = 15d - 20d; there is also excess power
at low frequences in the photometric data. Earlier
studies revealed photometric periods 0.284d - 0.4d
and violation of periodicity.
V987 Oph d = 0.02P. Min II 14.6. See V423 Oph.
V998 - V999 Oph
In the regi-
on of the globular cluster NGC 6171.
V1000 Oph See V822 Oph.
V1002 Oph Min II 15.2.
RRC type with twice shorter P is possible.
V1004 Oph See V822 Oph.
V1010 Oph Min II 6.46. P var. P = 0.661464d (JD 2415000 -
25000) [5738]; since JD 2425000 -
see Table, nonlinear term:
- 3.87d*10**-10*E**2.
Min I var.The light curve shape and the depth of
Min I var.
V1011 Oph See V822 Oph.
V1015 Oph D <= 0.23P, d < 0.02P; Min II 14.5.
V1017 Oph [Fe/H] = -1.25. P var? Max = 2437433.935 + 0.2343d*E
(JD 2437433 - 514) [3625]. During
JD 2442954 - 45140 - see Table.
According to [9037], P = 0.361d.
V1018 Oph Possibly eclipsing.
V1021 Oph delta(m) var. B - V: +0.42, +0.62.
V1022 Oph d = 0.06P:; Min II 15.95.
V1024 Oph Max = 2437433.559 + 0.5914d*E (JD 2437433 - 514)
[3625]. During JD 2442954 - 45140 -
see Table.
RR(B) type is possible; P =
= 0.371d satisfies the observations during
JD 2442954 - 44407.
V1026 Oph Max = 2437433.562 + 0.6563d*E (JD2437433 - 514)
[3625]. During JD 2442954 - 45140 -
see Table.
V1028 Oph See V822 Oph.
V1032 Oph P > 1.0d is not excluded.
V1033 Oph Max = 2437433.714 + 0.4845d*E (JD 2437433 - 514)
[3625]. During JD 2442954 - 45140 -
see Table.
V1035 Oph Max = 2437433.388 + 0.6100d*E (JD 2437433 - 514)
[3625]; during JD 2442954 - 45140 -
see Table.
V1039 Oph P = 0.3166d is possible.
V1040 Oph The light curve shape
var.
V1041 Oph [Fe/H] = - 1.06.
V1042 Oph See V1040 Oph. Max = 2437433.633 + 0.5528d
(JD 2437433 - 514) [3625]. During
JD 2442954 - 45140 - see Table.
V1052 Oph Max = 2437433.537 + 0.7546d*E (JD 2437433 - 514)
[3625]; during JD 2442954 - 45140 -
see Table.
V1054 Oph VB Wolf 630AB (A 9.76m V, 12.47mu; B 9.78m V; A =
= 0.22", Porb = 1.71665 yr; C = Wolf 629, 11.70m V,
14.75mu, dM4, 72", D = vB8, 16.7m V, 221",
common mu). mu = 1.19", ro = 222deg. Lx/Lopt(V) = 0.05.
V1072 Oph P var. Max = 2439025.31 + 0.444715d*E (JD 2438500 -
39025); since JD 2442800 - see
Table.
V1075 Oph Red.
V1077 Oph P var. Max = 2438614.40 + 0.373926d*E (JD 2438200 -
700); Max = 2442871.516 + 0.37384d*E (JD 2442810 -
910): Max = 2442983.345 + 0.373911d*E (JD 2442920 -
3330); since JD 2443330 - see
Table.
V1089 Oph VB AB (B 16.4m, 2", 45deg).
V1099 - V1100 Oph
Red.
V1111 Oph OH, H2O, SiO maser.
V1120 Oph Min II 14.3.
V1121 Oph Soft X-ray sour-
ce.
V1135 Oph [Ca/H] = -0.74.
V1141 - V1142 Oph
P var? The light
curve shape var?
V1146 Oph P = 185.2d is possible.
V1153 Oph P = 153.0d is possible.
V1157 Oph B - V: +0.42, +0.66.
V1161 Oph P = 0.49d is possible [6438].
V1168 Oph See V1141 Oph.
V1170 Oph P = 360d: is possible [6438].
V1174 Oph See V1141 Oph.
V1176 Oph P = 269.0d is possible.
V1179 Oph See V1141 Oph.
V1185 Oph Other possible ele-
ments: Max = 2435630 + 177d*E [0001].
V1195 Oph One more Max 2435637 (1956).
Type M is possible.
V1203 Oph P = 315d is possible [6438].
V1204 Oph P = 144d: or P = 191d: are possi-
ble.
V1235 Oph UV type is possible.
V1240 Oph P = 0.42136d is possible.
V1244 Oph See V1141 Oph.
V1258 Oph P var?
V1261 - V1262 Oph
The light curve is not typical
for the P in the Table [6438].
V1276 Oph [Ca/H] = -0.1.
V1296 Oph [Ca/H] = -0.9.
V1299 Oph See V1141 Oph.
V1300 Oph P = 235d: is possible.
V1305 Oph Min II 17.9:.
V1307 Oph See V1141 Oph. Spu-
rious period? [6438].
V1323 Oph P var?
V1332 Oph [Ca/H] = -0.64.
V1348 Oph See V1141 Oph.
V1355 Oph See V1141 Oph.
V1403 Oph P = 215d?
V1423 Oph See V1141 Oph.
V1426 Oph P var?
V1451 Oph P = 179.4d?
V1474 Oph P = 127d:?
V1491 Oph P = 328.0d?
V1492 Oph See V1141 Oph.
V1505 Oph P = 86d:?
V1512 Oph See V1141 Oph.
V1526 Oph P = 0.29745d?
V1532 Oph P = 144.4d?
V1534 Oph P = 198.8d?
V1554 Oph P = 136.0d?
V1568 Oph P = 275.5d?
V1571 Oph P var?
V1573 Oph Type E?
V1583 Oph P - spurious?
V1616 Oph Type E?
V1628 Oph See V1141 Oph.
V1637 Oph [Ca/H] = -0.44.
V1661 Oph See V1141 Oph.
V1666 Oph P = 154.2d?
V1676 Oph Close optical compa-
nion?
V1682 Oph P = 118.0d?
V1687 Oph Type CW?
V1702 Oph P = 121d?
V1705 Oph P var?
V1710 Oph P = 0.37422d?
V1731 Oph See V1141 Oph.
V1736 Oph P = 143.8d?, P = 244.5d?
V1744 Oph P = 191.6d?
V1748 Oph A var. Type CW?
V1754 Oph P = 128.4d?
V1768 Oph See V1141 Oph.
V1775 Oph Type EW?
V1793 Oph P = 170d:?
V1803 Oph The star is not SVS 438.
V1805 Oph See V1141 Oph.
V1811 Oph Min II 17.9:.
V1814 Oph P = 160.4d?
V1822 Oph P var?
V1829 Oph P = 143.2d?
V1840 Oph V 12 (NGC 6333 = M9). Cluster
member.
V1841 Oph See V1141 Oph.
V1845 Oph V7 (NGC 6333 = M9). Cluster
member.
V1853 Oph See V1141 Oph.
V1860 Oph [Ca/H] = - 0.49.
V1861 Oph P = 142.0d?
V1864 Oph V3 (NGC 6333 = M9). Cluster
member.
V1886 Oph See V1141 Oph.
V1889 Oph P = 316.0d?
V1895 Oph See V1141 Oph.
V1905 Oph P = 149.0d?
V1919 Oph P = 102.8d?, P = 227.0d?
V1939 Oph P = 330.0d?
V1946 Oph See V1141 Oph.
V1952 Oph P = 248.0d?
V1953 Oph P = 199d:?, P = 235d:?
V1954 Oph P = 159.6d?
V1973 Oph P = 0.24154d?
V1989 Oph A var?
V1990 Oph P = 121d:?
V1991 Oph See V1141 Oph.
V1994 Oph P = 170.0d?
V1998 Oph P = 270.5d?
V2002 Oph See V1141 Oph.
V2003 Oph [Ca/H] = -0.96.
V2009 Oph V5 (NGC 6356). Cluster member.
V2010 Oph [CA/H] = -0.79.
V2016 Oph [CA/H] = -0.96.
V2042 Oph P var. Max = 2430146.478 + 0.5385d*E (JD 2429100 -
30202); since JD 2436700 - see
Table.
V2048 Oph SB 2 [6598]. See V423 Oph.
Along with irregular light vari-
ations typical for be stars tHere are rapid flares
with the amplitudes up to 1.8m (lambda eff = 5800 A)
[6150]. It is not excluded that the flares occur on a
fainter companion of the system.
V2051 Oph Usually - 15.0m with strong fli-
ckering of brightness (up to 0.4m is 5 minutes) and
rare flares. At the same time the eclipses are ob-
served with depth to 2.5m with the elements: Min =
= 2444787.32124 + 0.062427865d*E [9550]; D =
= 0.0088P:, d = 0.0065P.
V2058 Oph In the
dark nebula in the RO Oph region.
V2059 Oph See V2058 Oph.
V2061 Oph In the region of
the globular cluster NGC 6171 (M 107).
V2062 - V2064 Oph
See V2058 Oph.
V2101 Oph In a dark nebula.
V2102 Oph In the region of
the globular cluster NGC 6293.
V2105 Oph Vr = 100 km/s.
V2106 Oph = -102 km/s.
V2108 Oph H2O, SiO maser.
V2112 Oph The primary oscillation with A1 = 0.0172m
(See Table) is superimposed by the secondary one
(A2 = 0.0061m) with the elements: Max =
= 2444114.531: + 0.1449461d*E.
V2116 Oph X-ray pulsar. The pulse period is dec-
reasing: 135s (1971), 112.076s (1979), 109.668s
(1980) [9553]. The spin-period may be twice
longer.
V2118 Oph Probably rapidly rotating single spotted F type star.
Max brightness epoch is given.
V2119 Oph In the region of the globular cluster
NGC 6284. Not a member of the cluster.
V2120 Oph V6 (NGC 6284). See V2119 Oph.
V2121 Oph V10 (NGC 6284). See V2119 Oph.
V2122 Oph See V2119 Oph.
V2123 Oph V11 (NGC 6284). See V2119 Oph.
V2124 Oph See V2119 Oph.
tet Oph SB 1 (Porb = 11.44d [6597]).
The basic oscillation (See Table) is superim-
posed by oscillations with the periods: P1 = 0.092551d,
P2 = 0.069452d, P3 = 0.0555d, P4 = 0.0464d, P02 =
= 0.137255d, P13 = 0.13845d, P24 = 0.13990d, P03 =
= 0.09185d.
hi Oph SB 1 (Porb = 138.8d [9558]).
ome Oph P = 1.5d?
R Ori SC 5/9.5 E. P var. Max = 2399420 + 378d*E (JD
2395600 - 99500); Max = 2412687 + 378.1d*E (JD
2403200 - 12700); Max = 2414230 + 366.5d*E (JD
2413800 - 16800); Max = 2417943 + 378.1d*E (JD
2416800 - 21350); Max = 2421352 + 384.9d*E (JD
2421350 - 24100); since JD 2424100 -
see Table.
S Ori VB A (B 10.9m, 47", 228deg). SiO maser. P var.
Max = 2404538 + 412.00d*E (JD 2404520 - 13600);
Max = 2414014 + 427.15d*E (JD 2414000 - 19150);
Max = 2419567 + 416.11d*E (JD 2419570 - 22890);
Max = 2423312 + 407.10d*E (JD 2423320 - 31050);
Max = 2431454 + 438.53d*E (JD 2431500 - 39000)
[3765]; since JD 2439000 - see
Table.
T Ori In the T-associa-
tion of the Orion nebula. Connected with a cometa-
ry nebula.
U Ori SiO, OH, H2O maser. P var. Max = 2409881 +
+ 374.5d*E (JD 2409800 - 15900); Max = 2415871 +
+ 367.9d*E (JD 2415900 - 21000); Max = 2421016 +
+ 376.0d*E (JD 2421000 - 29300); Max = 2428164 +
+ 368.3d*E (JD 2428100 - 32900) [0960]; Max =
+ 2433336 + 372.7d*E (JD 2432900 - 43800);
since JD 2443800 - see Table.
V Ori P var. Max = 2413656 + 264.8d*E (JD 2411800 - 18700);
Max = 2418987 + 271.7d*E (JD 2418700 - 24600);
Max = 2424695 + 263.7d*E (JD 2424600 - 29400)
[0960]; Max = 2430769 + 269.9d*E (JD 2430700 -
36200); since JD 2437700 - see
Table.
W Ori Mean magnitude varies with P = 2450d.
Z Ori Min II 9.9; d = 0.013P.
RS Ori P var. Max = 2428073.205 + 7.566836d*E (JD 2416500 -
33000); since JD 2435000 - see
Table.
RT Ori Mean magnitude varies with P = 3200d.
RU - RW Ori In the region of
the nebula IC 434.
RX Ori In the region of the Orion nebula T-association.
RZ - TW Ori
See RX Ori.
TX Ori VB A (B = TY Ori, 42.4", 45deg); see RU Ori.
TY Ori VB B (A = TX Ori); see RU Ori.
TZ Ori See RU Ori.
UW Ori Min II 11.6.
UY - UZ Ori
See RX Ori.
VV Ori Min II 5.50; dI = 0.055P; dII = 0.064P.
There is third component
in the system (Porb = 119.09d [8045]).
VW - VX Ori
See RX Ori.
VY Ori VB A (B = 16.6mV, 16", 135deg). See RX Ori.
VZ - WW Ori
See RX Ori.
WX Ori VB A (B 17m, 11", 10deg). See RX Ori.
WY - XY Ori
See RX Ori.
XZ Ori The periodicity in light variations is possible.
See RX Ori.
YY Ori Emission. See RX Ori.
YZ - AF Ori
See RX Ori.
AG Ori VB A (B 16.4mV, 16", 185deg). See RX Ori.
AH - AL Ori
See RX Ori.
AM Ori VB A (B 20.3mV, 3.5", 320deg). See RX Ori.
AN - AQ Ori
See RX Ori.
AR Ori VB A (B 2", 240deg). See RX Ori.
AS - AU Ori
See RX Ori.
AV Ori VB A (B 18.7mV, 6", 305deg). See RX Ori.
AW - BF Ori
See RX Ori.
BG Ori See RU Ori.
BH Ori See RX Ori.
BK Ori P var. Max = 2422016 + 338.0d*E (JD 2413550 - 22100);
Max = 2428880 + 326.5d*E (JD 2422300 - 28880);
Max = 2429940 + 345.3d*E (JD 2428880 - 29940);
Max = 2432892 + 327.7d*E (JD 2429940 - 32900);
Max = 2438800 + 346.3d*E (JD 2432900 - 38800);
since JD 2438800 - see Table.
BM Ori See RX Ori. In the cluster NGC
1976. Orion Trapezium
member: teta**1 Ori B (A = V1016 Ori; B 8.7", 32deg;
C 5.13m, 13.1", 131deg; D 6.70m, 21.6", 96deg). d = 0.05P;
Min II 7.98.
Shape of the light curve and
depths of minima vary.
BO - BP Ori
See RX Ori.
BS - CH Ori
See RX Ori.
CI Ori VB A (B 9.70m, 12.9", 88deg).
CM Ori P var?
CN Ori Porb = 0.163097d.
Light curve is superposed by oscillations with
the following elements: Max0 = 2444941.5032 +
+ 0.163097d*E (A0 = 0.2m), Max1 = 2444941.573 +
+ 0.15946d*E (A1 = 0.1m) [9471].
Sometimes smaller
rapid light oscillations are also observed with peri-
ods 24.3s - 29.5s (A<1%).
CO Ori Member of the T-association
CO Ori. VB A (B 13m, 1", 280deg).
CP Ori Min II 11.2. P var [2545].
CT Ori SRD? P = 68d? [9496].
CW Ori Min II 13.2.
DK Ori See RX Ori. VB (ro < 3").
DL Ori See RX Ori.
DM Ori See RX Ori.
DN Ori Min II 9.9; d = 0.026P. P var. Min I = 2428497.51 +
+ 12.9649d*E (JD 2425200 - 28600); since
JD 2435570 - see Table.
DY Ori B - V: +0.58, +1.72.
EG Ori d = 0.086P. P var?
EQ Ori Min II 10.3. P var. Min I = 2425889.706 + 1.74608d*E
(JD 2425600 - 26700) [2839]; Min I = 2429219.467 +
+ 1.74611d*E (JD 2427700 - 31000) [0001];
since JD 2431000 - see Table.
ER Ori VB A (B 13.6", 0deg). Min II 9.97. P var. Min I =
= 2426336.6485 + 0.4233955d*E (JD 2426330 - 33920)
[0279]; Min I = 2434765.6306 + 0.42340620d*E
(JD 2433920 - 35475) [2278]; Min I = 2436508.7851 +
+ 0.4234009d*E (JD 2435475 - 40000) [3787];
since JD 2440000 - see Table.
Shape of the light curve
varies.
ET Ori Min II 11.3. P var?
EW Ori Min II 10.5; Min II - Min I = 0.529P.
In the region of the open cluster
CR 70.
In [0007] Min II are accepted
to be Min I, and vice versa (Min II - Min I = 0.47P).
for decisive choice of the Min I epoch photoelect-
ric observations are necessary. P var? Min II =
= 2429974.810 + 6.9368005d*E [0007]; since
JD 2430000 - see Table.
EY Ori Min II 9.54; d = 0.003P. See RX Ori. P var.
Min I = 2427310.420 + 16.787450d*E [0007];
since JD 2427500 - see Table.
EZ Ori See RX Ori.
FF Ori Min II 10.3.
FH Ori d = 0.035P. P var.
FI Ori VB A (B 10.5m, 5", 323deg).
Shape of the light
curve varies, probably periodically [3790, 5475].
FK Ori P var. Min = 2427773.390 + 1.947447d*E (JD 2426900 -
37500); since JD 2437500 - see
Table.
FL Ori P var. Min = 2427452.271 + 1.550971d*E (JD2427450 -
29600) [3115]; Min = 2430400.649 + 1.55093d*E (JD
2429600 - 30400);Min = 2432517.755 + 1.550991d*E
(JD2430400 - 32900); Min = 2434459.571 + 1.550965d*E
(JD2432900 - 35050); Min = 2436649.568 + 1.550995d*E
(JD2435050 - 40600); since JD2440600 -
see Table.
FO Ori Min II 9.7; d = 0.005P.
FR Ori Min II 11.1.
FT Ori Min II 9.60; DII = 0.08P; Min II - Min I = 0.73P. P var.
Min I = 2433009.553 + 3.150404d*E (JD2426380 - 38000)
[2758]; since JD2438000 - see
Table.
The period of apsidal motion 520 + - 100 years [7358].
FU Ori Member of FU Ori T-association. In the dark globule B35.
Connected with a bright cometary nebula and the bright
hydrogen nebula S 280. Light maximum was in summer
1937. IN 1980 - 10.6m B.
FZ Ori Min II 11.2.
GG Ori Min II 11.1; Min II - Min I = 0.427P.
GP Ori SC 7/8 - .
GQ Ori VB A (B 9.7m, 31", 324deg).
GW Ori In the T-association CO Ori.
GX - GY Ori
See GW Ori.
GZ - HH Ori
See RX Ori.
HI Ori See GW Ori.
HK Ori See GW Ori.
Connected with a bright cometary nebu -
la. CO, CH, OH emission.
HL Ori See RX Ori.
HM Ori See GW Ori.
HN - LY Ori
See RX Ori.
LZ Ori VB B (A 10.3m; B 14.1", 219deg). See RX Ori.
MM - NT Ori
See RX Ori.
NU Ori See RX Ori. In the nebula NGC
1982. Dust shell.
NV - NX Ori
See RX Ori.
NY Ori VB B (A = V566 Ori; B 5", 135deg). See RX Ori.
NZ - OR Ori
See RX Ori.
OT - PP Ori
See RX Ori.
PQ Ori See RU Ori.
PR - PT Ori
See RX Ori.
PU Ori See RU Ori.
PV - PW Ori
See RX Ori.
PX Ori = + 298 km/s [9511]. See RX Ori.
PY - QQ Ori
See RX Ori.
QR Ori In the region of T-associa -
tion FU Ori.
QT Ori P var?
Elements given in the
Table are valid in the interval JD2429640 - 35550.
V340 Ori Epoch of Min brightness is
given.
V343 Ori Min II 11.0.
Shape of the light curve And depth of
Min II varY.
V347 - V349 Ori
See RX Ori.
V353 - V358 Ori
See RX Ori.
V359 Ori See RX Ori.
Epoch of Min HEI line intensity is given.
According to [9512], P = 14.612d.
V360 Ori See RX Ori.
V361 Ori VB C (A 4.8m; B 6.1m, 52.4", 93deg; C 129", 97deg).
See RX Ori.
V362 - V369 Ori
See RX Ori.
V370 Ori See GW Ori.
V371 Ori mu = 0.28", ro = 238deg.
V372 - V379 Ori
See RX Ori.
V380 Ori In the nebula NGC 1999. See
RX Ori. Spectrum description
[4002]. OH, CH emission.
V381 Ori See RX Ori.
V382 Ori P var. MAX = 2431146 + 227.8d*E (JD2429300 - 31200);
Mean period is
given in the Table (JD2428100 - 33700).
V383 - V391 Ori
See RX Ori.
V393 - V428 Ori
See RX Ori.
V432 Ori delta(S) = 0.
V435 Ori P var. Max = 2430350 + 186d*E (JD2429600 - 30730);
Max = 2431373 + 186d*E (JD2431370 - 3250) [2279];
since JD2434000 - see Table.
V436 - V439 Ori
See GW Ori.
V441 Ori See GW Ori.
V442 Ori VB A (B 16.6m, 20", 73deg). See GW Ori.
V443 - V448 Ori
See GW Ori.
V449 Ori See GW Ori.
In [8289] was con -
sidered as an EW type variable with the elements:
Min I = 2430259.622 + 0.441990d*E (JD2430250 - 5550),
14.8m - 15.7m pg.
V450 Ori See GW Ori.
V452 - V458 Ori
See GW Ori.
V460 - V461 Ori
See GW Ori.
V463 - V465 Ori
See GW Ori.
V466 Ori See RX Ori.
V467 Ori See GW Ori.
V468 Ori See RX Ori.
V470 Ori See RX Ori. Star Pi 1411. Near
to WY Ori = Pi 1396.
V473 - V475 Ori
See RX Ori.
V476 - V477 Ori
In the regi-
on of the open cluster lambda)Ori.
V478 Ori See RX Ori.
V479 Ori See RX Ori.
In the infrared A>1.5m.
V480 Ori See V479 Ori.
V481 - V482 Ori
See RX Ori.
V484 Ori See RX Ori.
In the infrared A>1.0m.
V485 Ori See V484 Ori.
V486 - V488 Ori
See RX Ori.
V489 - V491 Ori
See V484 Ori.
V492 Ori See RX Ori.
Northern component of the close pair of infrared stars.
In the infrared A = 1m.
V493 Ori See V484 Ori.
V494 Ori See RX Ori.
V495 Ori See RX Ori.
Close binary (ro =
= 0.24"). It is unknown which of the components varies.
V496 - V497 Ori
See V484 Ori.
V498 Ori See RX Ori.
V500 - V502 Ori
See RX Ori.
V504 Ori Min II 15.4.
V505 Ori See RU Ori.
V507 - V511 Ori
See RU Ori.
V514 Ori See RU Ori.
V516 Ori Max = 2430325 + 139d*E (JD2430250 - 5350); P = 70d
(JD2435350 - 550).
V519 Ori Min II 12.9.
V522 - V523 Ori
See RU Ori.
V525 Ori Min II 14.7.
V526 Ori See QR Ori.
V529 Ori NOVA Ori 1678?
Recurrent
outburst was possibly observed at 1894 [2866]. Ear -
lier the object was considered as nova Ori [1667
2862, 2863, 2867, 2868], its existence being consi -
dered as doubtful [3813].
V537 Ori See V476 Ori.
V538 - V542 Ori
See RX Ori.
V544 - V547 Ori
See RX Ori.
V548 - V549 Ori
See V476 Ori.
V550 - V557 Ori
See RX Ori.
V559 - V571 Ori
See RX Ori.
V572 Ori See V476 Ori.
V573 - V582 Ori
See RX Ori.
V584 - V594 Ori
See RX Ori.
V595 Ori See RU Ori.
V596 Ori See V476 Ori.
V597 Ori See RU Ori.
V598 Ori See V476 Ori.
V599 Ori See RX Ori.
V600 - V608 Ori
See RU Ori.
V610 - V611 Ori
See RU Ori.
V612 Ori See RU Ori. VB A (B 4.2", 330deg).
V614 Ori See QR Ori.
V615 - V623 Ori
See RU Ori.
V625 - V632 Ori
See QR Ori.
V634 - V639 Ori
See QR Ori.
V640 Ori d <= 0.02P.
V641 Ori Min II 14.5.
V642 Ori d = 0.05P?.
V643 Ori P = 26.2075d?
V647 Ori Min II 11.9. P var. Min I = 2418005.035 + 0.977575d*E
(JD2414660 - 23230); since JD2423230 -
see Table.
V648 Ori Min II 12.2.
V649 Ori See GW Ori. VB A (B 15m, 2", 0deg).
V650 Ori See V476 Ori.
V652 Ori See RX Ori.
V654 - V659 Ori
See RX Ori.
V667 Ori Min II 15.0.
V676 - V684 Ori
See RX Ori.
V685 Ori See RX Ori. A(U) = 1.0m.
V686 - V712 Ori
See RX Ori.
V713 Ori See RX Ori. A(U) = 4.0m.
V714 - V717 Ori
See RX Ori.
V718 Ori See RX Ori.
Probably the sf-component of a ve -
ry close pair.
V719 - V736 Ori
See RX Ori.
V737 Ori See RX Ori. A(U) > 2.4m.
V738 - V739 Ori
See RX Ori.
V740 Ori See RX Ori. A(pg) > 4.0m.
V741 - V742 Ori
See RX Ori.
V744 - V757 Ori
See RX Ori.
V758 Ori See V740 Ori.
V759 - V766 Ori
See RX Ori.
V767 Ori See RX Ori. A(U) = 1.5m.
V768 Ori See RX Ori.
V770 - V777 Ori
See RX Ori.
V778 Ori See RX Ori. A(pg) = 1.6m.
V779 Ori See RX Ori.
V780 Ori See V685 Ori.
V781 - V782 Ori
See RX Ori.
V783 Ori See RX Ori. A(pg) = 3.0m.
V784 - V806 Ori See RX Ori.
V807 Ori See V740 Ori.
V808 Ori see RX Ori.
V810 - V835 Ori
See RX Ori.
V836 Ori See RX Ori. A(U) > 1.5m.
V837 Ori See V740 Ori.
V838 - V839 Ori
See RX Ori.
V840 Ori See RX Ori. A(pg) = 0.7m.
V841 - V854 Ori
See RX Ori.
V855 Ori See RX Ori. A(U) > 2.0m.
V856 Ori See RX Ori.
V857 Ori See RX Ori. A(pg) > 5.0m.
V858 - V866 Ori
See RX Ori.
V867 Ori See RX Ori. A(pg)>3.0m.
V868 - V875 Ori
See RX Ori.
V876 Ori See RX Ori.
Southem component of a close pair.
V877 - V882 Ori
See RX Ori.
V883 Ori See RX Ori.
In the apex of a cometary nebula.
V884 - V885 Ori
See RX Ori.
V886 Ori See RX Ori. A(pg) > 3.5m.
V888 - V891 Ori
See RX Ori.
V892 Ori See RX Ori. Sou-
thern component of a pair (ro = 3").
V893 Ori See RX Ori. A(U) = 2.0m.
V894 - V899 Ori
See RX Ori.
V900 Ori See RX Ori. A(pg) > 2.5m.
V901 Ori See RU Ori.
V902 Ori See RX Ori.
V904 - V909 Ori
See RX Ori.
V916 Ori P = 0.28297d? Member
of the open cluster NGC 2169.
V917 Ori Member of the open
cluster NGC 2169.
V918 - V924 Ori
See RX Ori.
V926 - V935 Ori
See RX Ori.
V937 - V939 Ori
See RX Ori.
V941 - V943 Ori
See RX Ori.
V945 - V952 Ori
See RX Ori.
V953 Ori See RU Ori.
V956 - V957 Ori
See RU Ori.
V958 Ori See RX Ori.
V960 Ori See RU Ori.
V961 Ori See RX Ori.
V964 Ori P var. Max = 2415800.389 + 0.5046772d*E (JD
2415800 - 21010); Max = 2424500.446 + 0.50466477d*E
(JD2424500 - 30500); since JD2431500 -
see Table.
V965 - V992 Ori
See RX Ori.
V994 - V997 Ori
See RX Ori.
V998 Ori mu = 0.28", ro = 221deg.
V999 - V1002 Ori
See RX Ori.
V1003 Ori mu = 0.272", ro = 60.8deg.
V1004 Ori VB A (B 10.57m, 37", 204deg); SB (P = 2.74d).
V1005 Ori The range of light
variations (characteristic for BY Dra type varia -
bility) between the flares is given in the Table;
the amplitude of the flares A(U) can reach 3.2m.
V1006 - V1007 Ori
See RX Ori.
V1016 Ori See RX Ori. In the cluster NGC
1976. Orion Trapezium
member: teta1 Ori A (B = BM Ori, 8.7", 32deg; C 5.13m,
13.1", 131deg; D 6.70m, 21.6", 96deg). d = 0.001P.
V1017 - V1020 Ori
See RX Ori.
V1022 Ori See QR Ori.
V1028 Ori P = 6d?
V1029 Ori See RX Ori.
V1030 Ori See RU Ori. VB (sigma Ori) E (A 4.1m; B 5.1m, A =
= 0.247", P = 170yr; C 8.79m, 11.2", 238deg; D 6.66m,
12.9", 84deg; E 41.6", 61deg). Min I (HeI) = 2442802.48 +
+ 1.19080d*E.
Unusual helium variable. Epoch of
Min I brightness is given in the Table (Min II 6.71,
Min II - Min I = 0.43P). This epoch is being observed
by 0.18P later than the epoch of minimum strength
of the HeI lambda 4026 A line. According to [9524], light
minima are due to "eclipses" of the star surface
by two isolated clouds (consisting of hydrogen And
helium), which are located almost oppositely near
the intersections of the magnetic And rotational
equator.
V1031 Ori VB (0.159", 104deg, 1980.7). Min II 6.32; DII = 0.017P.
V1034 Ori Epoch of light minimum
is given.
V1035 - V1045 Ori
See RX Ori.
V1046 Ori See RX Ori. SB 1. Min II 6.58.
Possibly an ellipsoidal variable, its light variations
being superimposed by light variations of the
primary component of SX Ari type: Min (HeI) =
= 2442812.23 + 0.9015d*E [8054].
V1047 - V1050 Ori
See RX Ori.
V1052 - V1053 Ori
See RX Ori.
V1054 Ori See V1034 Ori. P = 8.596d?, P = 8.674d?
V1055 Ori P(X) = 5.2d [9528].
V1056 Ori VB A (B 9.8m, 28.7", 58deg).
V1058 - V1084 Ori
See RX Ori.
alf Ori VB A (B 14.5m, 39.8", 110deg). Min = 2410600 + 2070d*E
(1840 - 1929) [1012]. Since 1929 -
see Table.
The main variation is superimposed by the waves
with P = 200 - 400d. Dust-gaseous shell (r = 50")
[9529].
del Ori VB A (A 0.217", 144deg, 1980; B 14.0m, 33.1", 227deg;
C 6.84m, 53.5", 359deg). See epsilon Ori. Min II 2.20.
Apsidal motion (P = 210 yr).
Shape
of the light curve varies. The intrinsic brightness va-
riability of the components is possible.
eps Ori Orion Belt cluster
member.
eta Ori VB Aab (AC 0.037", 111deg, 1979.0, P = 9.219 yr [9535];
B 4.8m, 1.60", 76deg, 1976.0; C 9.4m, 115", 51deg). EA/DM.
Min II 3.57. The range of combined
light variation of the components AAb (SB 2, P =
= 7.989268d), AC, and B is given in the Table. Out-
side eclipses there are sinusoidal light variations
of the system with A(V) = 0.05m due to pulsations of
the component Ab [9535] with P = 0.30197d [9536] or
0.30145D [9537]. According to [8566] these variations
were not observed between 1970 and 1976.
pi 5 Ori Min II 3.73.
The period is improved using radial velocities
[4627].
psi Ori VB A (B 11.1m, 2.7", 323deg; C 13.88m, 83", 196deg).
Min II 4.58.
The period is determined on the base of radi-
al velocities [9541].
R Pav Pvar. Max = 2411219 + 228.34d (JD2411000 - 18500);
Max = 2418527 + 230.95d*E (JD2418500 - 30000);
since JD2430000 - see Table.
S Pav P var. Max = 2421479 + 389.64d*E(JD2421000 - 31000);
since JD2431000 - see Table. delta(m)
var strongly.
Min II is
sometimes observed after Max I.
T Pav P var. Max = 2413328 + 243.45d*E(JD2405700 -
25500); Max = 2425499 + 245.11d*E(JD2425500 -
32500); since JD2432500 - see
Table.
V Pav VBA (B 14.0m vis, 15", 327deg). Mean
brightness var, P2 = 3735d, 9.7m - 10.7m.
W Pav P var. Before JD2431000 Max = 2413778 +
+ 282.92d*E; since JD2431000 -
see Table.
RT Pav Mean light var, 10.4m - 11.1m 1649,
P2 = 757d.
SU Pav P var. Max = 2430036 + 245.18d*E (JD2411000 - 30100)
[0001]; during JD247700 - 40000 -
see Table.
SX Pav mu alfa = + 0.0166s, mu delta = - 0.05".
TW Pav Before JD2420400 Max = 2417760 + 397.d*E.
YY Pav delta(m) var strongly.
P possibly is twice longer, in that case Min II 14.4.
AR Pav Depth of eclipses delta(m) = 2m B, d =
= 0.05P. Expanding shell.
BD Pav Only one out-
burst was observed [0629]. Brightness flickering. Ec-
lipses according to the elements Min I = 2444412.676 +
+ 0.1793015d*E, delta(m) ~ 0.5m [9191]. Out-
side outburst, 15.40m - 16.21m.
BF Pav Min II 11.9.
BI Pav Min II (delta(m) ~ 0.05m) is possible.
DF Pav Epoch of min is given. Light curve shape strongly var.
DN Pav delta(S) = 8:.
DW Pav Min II 16.3.
EG Pav Twice shorter P
is possible [0001].
EL Pav Min II 15.5.
EN Pav Elements
need confirmation.
EQ Pav Red.
FY Pav Min II? JD2436784.37.
HL Pav Blazhko effect?
HP Pav Min II 15.5.
HQ Pav Min II 12.7.
HY Pav Min II 12.1.
IL Pav RRC type is possible.
KR Pav Min II 14.1.
KZ Pav VB A (B 8.7m, 6.7", 119deg, 1971; C 9.2m, BC 1.0", 329deg,
1971). P var. Min = 2430448.617 + 0.949880d*E (JD
2416000 - 30000) [0001]; since JD2430000 -
See Table. Min II is present.
LL Pav Min II 15.1.
LO Pav Min II 16.5.
LR Pav Min II 15.3.
LT Pav Min II 12.2.
LV Pav Min II 14.3.
LY Pav Min II 14.9.
MQ Pav Epoch of Min is given. EW/KW type with
twice longer P is possible.
MR Pav Possible elements Max =
= 2436731.40 + 0.3737d*E [0001].
MS Pav Min II 14.1.
MW Pav d = 0.08P. Min II 8.92, dII = 0.11P.
NP Pav Deep Min II.
NW Pav [A/H] = -0.7.
kap Pav P var. Max = 2419619.38 + 9.0898d*E (JD2411930 -
22550); Max = 2425987.12 + 9.1028d*E (JD2422550 -
26980); Max = 2430530.67 + 9.0833d*E (JD2426980 -
31345); Max = 2433239.87 + 9.0956d*E (JD2431345 -
34045); Max = 2434693.11 + 9.0653d*E (JD2434045 -
37000); since JD2440000 - see
Table. [Fe/H] = 0.0/ - 0.4. Mo-
derately high Z coordinate (IZI ~ 240 pc provided
the period - luminosity relation for DCEP stars is va -
lid), low radial velocity. The period is not typical
for CW stars. Ca II emission was noticed in the spec -
trum.
lam Pav VB A (B 12.4m, 63.1", 206deg).
ro Pav The main light variation P1 (see Table) with a
semiamplitude delta(y) = 0.0069m is superposed by oscilla -
tions with P2 = 0.1131d (delta(y) = 0.0031m), P3 = 0.1612d
(delta(y) = 0.0029m).
R Peg OH, H2O, SiO maser.
P var. Max = 2396327 + 381.9d*E (JD2396300 -
2408200); Max = 2413012 + 371.4d*E (JD2413000 -
19800); Max = 2420092 + 379.77d*E (JD2420000 -
31100) [0960]; since JD2431100 -
see Table.
T Peg P var. Max = 2398452 + 371.0d*E (JD2398400 -
2408900); Max = 2413697 + 386.8d*E (JD2413600 -
18700); Max = 2421016 + 362.5d*E (JD2420900 -
28000) [0960]; Max = 2434343 + 376.0d*E (JD
2428300 - 34300); Max = 2440984 + 368.7d*E (JD
2434300 - 41000); since JD2441000 -
see Table.
U Peg Min II 9.73. P var.
There is a square term in the elements:
- 2.468D*10**-11*E**2. 0 - C = 0.00323d sin[(2pi/16330)E +
+ 0.418pi]. Shape of
the light curve varies.
W Peg SiO maser. P var. Max = 2413819 + 343.2d*E
(JD2413800 - 26600); Max = 2427162 + 345.5d*E (JD
2426600 - 32100) [0960]; Max = 2439690 + 348.75d*E
(JD2432300 - 39700) [0001]; since JD
2441400 - see Table.
X Peg P var. Max = 2414713 + 200.3d*E (JD2414700 - 21300);
Max = 2420105 + 204.3d*E (JD2420100 - 23800);
Max = 2423570 + 199.8d*E (JD2423600 - 31000) [0960];
Max = 2432006 + 208d*E (JD2431000 - 32100);
Max = 2434206 + 200.0d*E (JD2432100 - 39300);
since JD2438400 - see Table.
Z Peg P var. Max = 2415433 + 318.9d*E (JD2398800 -
2420550); Max = 2420207 + 328.0d*E (JD2420200 -
32000) [0960]; Max = 2432005 + 325.8d*E (JD2432000 -
37900); Max = 2437870 + 319d*E (JD2437500 - 40100);
Max = 2442086 + 328.0d*E (JD2440100 - 43100);
since JD2442100 - see Table.
RR Peg P var. Max = 2417582 + 268.3d*E (JD2416700 - 17850)
[0001]; Max = 2417859 + 260.8d*E (JD2417850 -
21000) [0960]; since JD2421000 -
see Table.
RS Peg P var. Max = 2415846 + 431.5d*E (JD2415800 - 18450);
Max = 2418434 + 404.1d*E (JD2418400 - 24200);
Max = 2424514 + 413.4d*E (JD2424500 - 34900) [0960];
Max = 2436496 + 403.4d*E (JD2435700 - 38600) [0001];
since JD2438500 - see Table.
RT Peg VB A (B 10.5m, 15.6", 291deg). P var. Max = 2423609 +
+ 215.0d*E (JD2416000 - 24300); Max = 2428149 +
+ 216.6d*E (JD2424300 - 32100); since
JD2432100 - see Table.
RU Peg VB A (B 12.5m, 12", 18deg); SB 2 (Porb = 0.3746d [9570]).
There are also light oscillations with P = 11.6s
and 50s [9571].
RV Peg Emission. Light curve
(1907 - 1973) [9572]. P var. Max = 2428735 + 388.4d*E
(JD2417000 - 32640); Max = 2430680 + 390.9d*E (JD
2430200 - 38900); since JD2438800 -
see Table.
RW Peg P var. Max = 2419393 + 208.4d*E (JD2412700 - 19400);
Max = 2421520 + 213.0d*E (JD2419390 - 21550); Max =
= 2427133 + 208.0d*E (JD2421500 - 27150);
since JD2427300 - see Table.
RX Peg P2 = 110d:.
RY Peg VB B (A = RZ Peg; B 20", 252deg).
RZ Peg VB A (B = RY Peg:20", 252deg). SC 6/9 - e. P var.
Max = 2423361 + 441.4d*E (JD2411400 - 26450); Max =
= 2431215 + 434.0d*E (JD2426400 - 33000);
since JD2433000 - see Table.
SS Peg P var. Max = 2416390 + 410.8d*E (JD2415500 - 20000);
Max = 2422235 + 423.8d*E (JD2420000 - 27000); Max =
= 2427270 + 403.4d*E (JD2427000 - 29000); Max =
= 2437218 + 416.35d*E (JD2428500 - 43000);
since JD2443000 - see Table.
SV Peg H2O emission.
SX Peg S 2.5/6 e. P var. Max = 2436043 + 306.56d*E (JD
2414800 - 38300); since JD2438300 -
see Table.
TU Peg P var. Max = 2417800 + 320.8d*E (JD2404300 - 18450);
Max = 2420730 + 328.4d*E (JD2418450 - 20800);
Max = 2428080 + 319.6d*E (JD2420800 - 31600);
since JD2432800 - see Table.
TW Peg H2O maser.
The basic light variation
with the period given in the Table is superimposed
by small oscillations with P = 94.13d.
TY Peg Min II 10.2. P var. Min I hel = 2419520.476 +
+ 3.0922754d*E (JD2412300 - 19600) [2389]; Min I hel =
= 2425918.348 + 3.092252d*E (JD2419600 - 26000)
[0001]; since JD2426000 - see
Table.
TZ Peg P var? Max = 2425892 + 213.7d*E (JD2410000 - 28000);
since JD2430000 - see Table.
UU Peg OH, H2O maser.
UW Peg According to [8837] P = 60d.
UX Peg P var. Min = 2428428.386 + 1.544618d*E (JD2422100 -
28430) [0230]; Min = 2431273.597 + 1.544632d*E
(JD2428420 - 34000) [0001]; since JD2434000 -
see Table.
VV Peg delta(S) = 8. P var. Max = 2420105.296 + 0.48837765d*E
(JD2420000 - 28900); Max = 2433217.268 + 0.48838307d*E
(JD2432800 - 38000) [3506]; since
JD2438000 - see Table.
VW Peg P = 2.341295d?
VX Peg The basic light variation is
superimposed by the secondary one with P = 80 - 90d:.
VZ Peg [Fe/H] = -1.75.
WW Peg P var. Max = 2433142 + 371.6d*E (JD2415670 - 33200)
[0001]; since JD2436800 - see
Table.
ZZ Peg Min II 12.5.
AE Peg P var. Max = 2415470.866 + 0.4967388d*E (JD2415500 -
21000); Max = 2426161.544 + 0.496725d*E (JD2425400 -
31500); Max = 2432632.809 + 0.496692d*E (JD2431500 -
36000) [0001]; during JD2436000 -
40000 - see Table. delta(S) = 6.3.
AG Peg SB 2 (Porb = 820d [9580]).
Maximum of brightness was in 1870, then the very
slow light decrease was observed that was superimposed
since 1935 by periodical light oscillations with A = 0.4m V
and P = Porb: Min = 2428250 + 827.d*E ( JD2428000-43000)[9587].
After JD2442300 the period probably has changed:
Min = 2442370 + 760d*E [9587]. In
1962 - 1979 the range of brightness was 7.95m - 8.55m V;
M - m = 0.50P.
Light minima corres-
pond to the epochs of inferior conjunction of M 3 III
component.
Spectrum var: Beq (1893 - 1919);
since 1922 the
spectrum is symbiotic one, the M star spectrum being
more noticeable.
Surrounded by a ra-
dio nebula with 1" half-power diameter.
AN Peg P var. Max = 2428045 + 274.1d*E (JD2424500 - 38500)
[9581]; since JD2438500 - see
Table.
AO Peg delta(S) = 4.3.
AQ Peg Min II 10.47; d = 0.030P. P var. Min I = 2424749.335 +
+ 5.548419d*E (JD2424000 - 34000) [0980];
since JD2434000 - see Table.
AT Peg Min II 9.04. P var. Min I = 2425862.337 + 1.1460988d*E
(JD2425800 - 37500) [0001]; Min I = 2437497.542 +
+ 1.146080d*E (JD2437490 - 40000) [6101]; Min I =
= 2440407*4370 + 1.1461007d*E (JD2440000 - 42400)
[0001]; since JD2442400 - see
Table.
AU Peg Cepheid in a
close binary system.
SB 1 (Porb = 53.319d, K1 = 41.8 km/s, gamma = -4.1 km/s,
E = 0.12 [9582]). [Fe/H] = 0.1.
P var. Max = 2428729.76 + 2.3978d*E (JD2426500 -
28750) [0916]; Max = 2433151.976 + 2.38934d*E (JD
2433150 - 35800); Max = 2439039.08 + 2.39079d*E
(JD2435800 - 39100) [0001]; since JD
2441700 - see Table.
THere is a square term in the ele-
ments given in the Table: +2.246d*10**-6*E**2.
The shape of the
light curve varies: 0.20P < M - m < 0.47P.
AV Peg P var. Max = 2416347.713 + 0.39036510d*E (JD
2414000 - 26500) [0752]; Max = 2426582.301 +
+ 0.39037015d*E (JD2426500 - 36000) [9584];
since JD2436000 - see Table. [Fe/H] =
= +0.02.
AW Peg d= 0.07P, Min II 7.60.
BB Peg Depth of Min II 0.60m.
There
is a square term in the elements given in the Table:
+ 2.3d*10**-11*E**2. dI = 0.05P; dII = 0.00P.
BF Peg P var. Max = 2426589.293 + 0.495796d*E + 2.8d*10**-9*E**2
(JD2426500 - 28800) [0522]; Max = 2433200.312 +
+ 0.495796d*E (JD2429400 - 33200) [0001]; Max =
= 2437583.343 + 0.495674d*E (JD2437500 - 39400)
[0001]; since JD2442650 - see
Table.
BG Peg P var. Min = 2427386.3705 + 1.952452d*E (JD2426000 -
35000) [3567]; Min = 2436453.509 + 1.95238d*E (JD
2435000 - 43500) [3624]; since JD2443500 -
see Table.
BH Peg P var. Max = 2426596.535 + 0.64101381d*E (JD
2426500 - 28200) [1038]; since JD2434400 -
see Table.
Blazhko effect. A var. Max (O - C) =
= 2442929.03 + 39.8d*N [9588]. (k - b)2 = 0.09; delta(S) = 5.
BI Peg Waves with
a cycle of 60 - 80d are superimposed.
BK Peg Min II 10.47.
BO Peg Min II 11.6. P var. Min I = 2427655.460 + 0.5804342d*E
(JD2426500 - 35100) [2263]; since JD
2444000 - see Table.
BP Peg P1 = 0.084510d; P1:P0 = 0.77. Beat
period Pb = 0.3698d [6604].
BU Peg Observations are represented by the elements in the
intervals JD2432000 - 34000, JD2438200 - 41400.
BX Peg Depth of Min II 0.62m; dI = 0.05P; dII = 0.00P.
P var. Min I = 2431323.278 + 0.2804238d*E (JD
2424700 - 39000) [0279]; since JD2439000 -
see Table.
BY Peg P var. Min I = 2424745.75 + 0.34193403d*E (JD
2424700 - 35400); since JD2435000 -
see Table.
CC Peg Min II 12.9.
CG Peg delta(S) = 2. P var?
CU Peg d = 0.010P. P var. Min = 2433895.463 + 3.8801345d*E
(JD2425500 - 34000) [0001]; Min = 2434221.392 +
+ 3.880196d*E (JD2434000 - 36500) [7929];
since JD2436500 - see Table.
CZ Peg Min II 13.9.
DF Peg Min II 9.2.
DG Peg P var. Max = 2425857 + 148.15d*E (JD2425500 -
33500); since JD2433500 - see
Table.
DH Peg P var. Max = 2414981.537 + 0.25550478d*E (JD
2414000 - 24000) [1158]; Max = 2427695.390 +
+ 0.2555107d*E (JD2424000 - 33500) [9590];
since JD2433500 - see Table. [Fe/H] =
= -0.9.
DI Peg Min II 9.59. P var. Min I = 2425644.315 + 0.7118144d*E
(JD2425500 - 30000) [2431]; Min I = 2437559.4096 +
+ 0.7118182d*E (JD2430000 - 40000) [9592]; Min I =
= 2440159.6796 + 0.71181417d*E (JD2440000 - 44500);
since JD2444500 - see Table.
DK Peg d = 0.04P. P var. Min = 2427745.388 + 1.631801d*E
(JD2427700 - 33700); since JD2433700 -
see Table.
DM Peg d = 0.03P; Min II 11.0.
DN Peg Mean brightness varies with cycles 800 -
1400d and A = 0.2m - 0.4m.
DO Peg P var. Min = 2434272.350 + 2.61394d*E (JD2428000 -
34700) [0485]; since JD2434700 -
see Table.
DV Peg Min II 12.1.
DY Peg P var. Max = 2432751.9624 + 0.072926372d*E (JD
2429000 - 38000); since JD2438000 -
see Table.
The basic pulsation is superimposed by the se -
condary one with P1 = 0.05570d [9594].
A var, M - m var (Pi = 0.2358d): 0.55m < A < 0.67m,
0.24P < M - m < 0.42P. delta(S) = 6.
DZ Peg P var. Max = 2429127.211 + 0.6073407d*E (JD
2419000 - 28800); Max = 2429127.189 + 0.6073761d*E
(JD2429100 - 33500); since JD2433500 -
see Table.
EE Peg Min II 7.06. The third body (Porb =
= 1464d, T0 = 2443120).
EF Peg VB B (A 14.0m; B 5", 305deg).
EH Peg d = 0.08P.
EQ Pega VB A (B = EQb Peg; A = 6.87", Porb = 359 yr, E = 0.20.
[9597]); mu = 0.560", P = 91.7deg. A (B) >= 1.4m.
EQ Pegb VB B (A = EQa Peg). See EQa Peg. A(U) >= 1.9m.
ET Peg delta(S) = 4.
EU Peg Min II 12.3.
EZ Peg On 1943 November 16 the spectrum of the star
was B [2875]; probably at that time the star had a
flare.
FL Peg Min II 14.0.
FU Peg Blazhko effect (Pi = 150d); A var;
15.2m <= Max <= 15.8m; 0.15P <= M - m <= 0.50P.
GH Peg Depth of Min II 0.13m.
GR Peg P var. Max = 2436492 + 69.93d*E (JD2436420 - 38740);
since JD2440470 - see Table.
GT Peg mu = 0.51", P = 96deg. Epoch of
the light minimum is given.
During the flares A(U) <
< 3.6m.
GV Peg delta(S) = 5:.
GW Peg Min II 15.1.
GX Peg SB 1 (Porb = 2.340939d [6103]).
GZ Peg VB A (B 10.6m, A3V, 32.7", 198deg).
HN Peg [Fe/H] = -0.09. Epoch of
light minimum is given.
The variability of emission in H
and K call lines with P = 4.63d was detected [9600].
HP Peg Vr = -381 km/s.
HR Peg S4+/1+ .
HZ Peg Min II 17.6.
II Peg mu = 0.575", p = 86.5deg. SB 1 (T0 = 2443030.396 + 6.724464d*E);
T0 is
the epoch of the inferior conjunction of K-star.
The epoch
of the distortion wave maximum is given in the Table.
Mean brightness of the system varies.
IK Peg SB 1 (Porb = 21.724d). Multipe-
riodicity [9609].
IM Peg SB 1 (Porb = 24.649d).
bet Peg VB A (B 11.2m, 109", 211deg).
eps Peg VB A (B 12.66m, 81", 325deg; C 8.65m, 140", 321deg).
Usually varies in the
range 2.29m - 2.44m V. On 1972 september 26/27 in the
interval 23h58m - 00h02m UT it was bright (0.7m V),
then at 00h09m UT decreased to 2.4m V [6875]. On
1847 November 5 the star was 3.5m, then the bright-
ness increased but on November 6 it was still fainter
than normal [9606].
tau Peg P2 = 0.04895d; PB = 0.4943d.
S Per See SU Per. OH, H2O, SiO maser.
In 1920 - 1969 there were secondary
waves with cycles of 300d - 700d And delta(m) ~ 1m [8630];
in 1935 - 1961 P1 = 807d, P2 = 930d [9694].
T Per Other periodi-
cities were noted. See SU Per.
U Per P var. Max = 2411683 + 316.10d*E (before JD
2422500); Max = 2422748 + 326.53d*E (JD2422500 -
34000); since JD2434000 - see
Table.
V Per VB A (B 14m, 28", 278deg).
W Per P2 = 2667d +- 460d is superimposed.
X Per 3U 0352 + 30. LX/Lopt = 10**-2. ADS 2859 A (B =
= V397 Per, M3III, 22.5", 12deg). SB.
IR excess. X-ray pulsar
(P = 13.93m).
Further
periodicities were noticed in X-ray, optical, spectro -
scopic observations: 22.4h, 308.33d, 580.7d.
Y Per P var. Max = 2414990 + 254.74d*E (JD2415000 - 18000);
Max = 2418049 + 246.25d*E (JD2418000 - 22000);
Max = 2422242 + 253.62d*E (JD2422000 - 41000);
since JD2441000 - see Table.
Z Per d = 0.028P; Min II 9.8.
P var. Min = 2418173.663 + 3.056422d*E (JD2415000 -
19000) [1961]; Min = 2425481.416 + 3.05636d*E
(JD2419000 - 31000) [0978]; since JD
2431000 - see Table.
RR Per P var. Max = 2424280 + 392.01d*E (JD2416000 - 28500);
since JD2428500 - see Table.
RS Per See SU Per. According to [1053], P =
= 152d.
RT Per Min II 10.67. P var. Min = 2411963.2995 + 0.84941322d*E
(JD2411317 - 19400); Min = 2419702.3124 +
+ 0.84940248d*E (JD2419400 - 29300); Min =
= 2429751.6066 + 0.84941274d*E (JD2429300 - 33000);
since JD2433000 - see Table.
RV Per Min II 10.4. P var. Min = 2417972.345 + 1.973489d*E
(JD2417000 - 25500); since JD2432500 -
see Table.
RW Per The light curve shape var,
d = 0.03P - 0.000P. Min II 9.78. P var. Before JD
2425720 Min = 2425720.0185 + 13.198910d*E;
Min = 2429217.5946 + 13.198399d*E (JD2425720 -
36700); since JD2436700 - see
Table.
RY Per d = 0.014P; Min II 8.65.
RZ Per S 3/7 e. P var. Before JD2430500 Max = 2415034 +
+ 353.19d*E; since JD2430500 -
see Table.
ST Per VB A (B 12.1m, 11.6", 6deg, 1928). d = 0.014P, Min II 9.62.
P var. Min = 2419030.5038 + 2.6483615d*E
(JD2418500 - 27000) [9740]; Min = 2429528.5897 +
+ 2.6483488d*E (JD2427000 - 34600) [2389]; Min =
= 2439091.716 + 2.648353d*E (JD2439000 - 42400);
since JD2442400 - see Table.
SU Per In the region of
the open cluster h, hi Per.
SV Per [A/H] = 0.6. SB 2, hot companion.
P var? Before JD2435000 Max = 2419055.145 +
+ 11.12875d*E [2431]; since JD2435000 -
see Table.
SX Per [A/H] = 0. The chart in
[8300]
SY Per In the region of
the open cluster NGC 1528.
TU Per delta(m), P var. Before JD2427200 Max = 2418572.288 +
+ 0.6070775d*E; Max = 2427119.334 + 0.6070643d*E
(JD2427200 - 36000); since JD2436000 -
see Table.
TV Per P2 = 1080d is superimposed.
TX Per [Fe/H] = -0.88. OH maser.
TZ Per VB A (B14m, 13", 290deg). Mu alfa = +0.012", mu delta = -0.050".
see SU Per.
UX Per [A/H] = -0.3.
UY Per [A/H] = -0.3. In
the region of the open clusters King 4, Czernik 8.
UZ Per P2 = 91d is superimposed.
VV Per Twice shorter
P is possible [0960].
VX Per See SU Per. [A/H] = -0.2. P var. Since
JD2431000 - see Table.
VY Per See SU Per. [A/H] = -0.3.
VZ Per VB A (B 16.9m pg, 17", 180deg). See DY Per.
WY Per P var. Min = 2425234.460 + 3.327126d*E (JD2421500 -
26000) [1072]; since JD2441500 -
See Table.
XX Per VB A (B 9.7m vis, 21", 176deg, 1909).
Mean brightness var, P = 4100d.
XY Per ADS 2788 AB (delta(mV) = 0.6m - 2.5m, 1.4", 75deg, SpA = A2II,
SpB = B6e). IR excess.
XZ Per Min II 11.6. P var? Min = 2425150.439 + 1.1516282d*E
(JD2425000 - 29000) [0522]; Min = 2437932.411 +
+ 1.1516347d*E + 0.005d sin (0.09091deg*E) (JD2432000 -
38000) [0001]; since JD2438000 -
see Table.
YZ Per See SU Per.
ZZ Per The coordinates
are possibly erroneous.
AB Per d = 0.045P; Min II 10.5. VB (delta(m) = 0.0m vis, 0.20", 86.4deg,
1978).
AD Per Mean brightness var, P = 2950d.
See SU Per.
AE Per P2 = 2150d is superimposed.
AG Per ADS 2990 A (B delta(m) = 2.0m, 0.9", 225deg, 1975; C 12.6m,
36", 118deg, 1948). The com-
bined brightness AB is given. Min II 7.00, DII = 0.10P,
dII = 0. Apsidal motion:
Min II - Min I = 1.01435d + 0.0884d sin (0.0278deg*E +
+49.1deg).
AR Per P var, nonlinear term: +1.18d*
*10**-11*E**2. [Fe/H] = -0.17.
AS Per delta(m) var, d (delta(b))/dt = -0.01m/yr.
AV Per P = 250 - 300d.
AW Per SB 2, companion B6V, delta(m) (companion - AW) =
= 2.8m vis.
AX Per Epoch of Min
is given. The variability with delta(m) up to 0.7m pg is
caused probably by the orbital motion. Outburst ac-
tivity is superimposed.
AY Per d = 0.009P.
BE Per In the region of
the open cluster CR 39.
BI Per In the region of
the open cluster Berk 9.
BL Per P = 125 - 130d.
BM Per [Fe/H] = -0.04.
BP Per Min II = Min I. See BE Per.
BU Per Max brightness var, P = 8.1yr
[1085]. See SU Per.
CC Per Min II 14.1.
CI Per P var (3.35d - 3.40d), possibly
with a period of 4000d. The
light curve shape var.
CK Per d = 0.05P:.
CM Per d = 0.052P. See CO Per.
CO Per In the region of
the open cluster Stock 2.
CR Per Elements need
confirmation. See CO Per.
CS Per See CO Per.
CZ Per See SU Per.
DE Per d = 0.01P?
DF Per See SU Per.
DG Per d = 0.021P.
DK Per The depth of Min II 0.05m. See SU Per.
DM Per Min II 8.02, DII = 0.17P.
Depths of Minima, the shape of Min II var.
See SU Per.
DO - DP Per
See SU Per.
DR - DU Per
See SU Per.
DV Per Min II 14.5.
DY Per In the region of
the open cluster Tr 2.
DZ Per Min II 14.7. See DY Per.
EL Per Before JD2428900 Max = 2427980 + 167d*E;
during JD2428900 - 31000 -
see Table.
EO Per IR excess?
ER Per Mean brightness var, P ~ 900d.
EU Per See ER Per.
EW Per Superimposed waves 70d - 180d.
See HS Per.
EX Per Min II 12.5.
FM Per VB A (B 12.1m, 3", 285deg). P var? Max = 2429982.268 +
+ 0.489199d*E (JD2428000 - 30600);
During JD2433700 - 36000 - see Table.
FR Per See SY Per.
FV Per Cycles 300 - 350d, 1800d:.
FX Per d = 0.04P. In the
region of the open cluster NGC 1582.
FY Per Possible periods 0.0702d,
0.4407d.
Photometric spectral type B1V.
FZ Per See SU Per.
GH Per P = 220d is possible.
GK Per SB 2 (sdBE + K2IVp).
The following ty-
pes of activity are being observed after the return
to the normal brightness: rapid irregular variations
(delta(m) ~ 0.1m in several minutes); irregular fluctuationS
from night to night (delta(m) up to 0.3m); slow irregular
variations (delta(m) = 1.5m in several dozen days); bursts
with light increase in 10d - 30d and decrease in
10d - 40d, delta(m) up to 3.5m, the mean interval between
bursts being delta(t) = 820d [9686, 9788]. according to
[10198], the radial velocities are represented with
the elements Max (Vr > 0) = 2444912.966 + 1.996803d*E
(Kabs = 124 km/s, Kem = 34 km/s). According to
[10199], the 2d variation is modulated with a period
of 0.131623d, Max (delta(Vr)) ~ 2443787.995 (Kabs =
= 15 km/s, Kem = 20 km/s). During a burst the sinu -
soidal modulation of X-ray flux was recorded,
Tmax = 24455555.67456 + 0.004066443d*E [9786].
ExpAnding envelope (0.454"/yr, 1948 - 1964;
0.432"/yr, 1964 - 1981, [9787]).
GP Per [A/H] = -0.5.
GQ Per According to [0021], Sp K0.
HQ Per [A/H] = -0.3.
HS Per In the region of
the open cluster Stock 4.
HV Per d ~ 0.03P.
HW Per Min II 13.3. Min II - Min I = 0.45P:.
HY Per Three of the four min in [1079] are not
satisfied with the elements.
HZ Per [A/H] = - 0.8. B_V: + 1.93, + 2.34.
II Per Min II 13.6. In
the region of the open cluster NGC 1582.
IK Per Min II 11.6.
IM Per Min II 12.7.
The elements need confirmation. See BE Per.
IO Per H2O maser.
IP Per IR excess.
IQ Per dI = 0.02P. Min II 7.88, DII = 0.12P, dII = 0.03P, Min II -
- Min I = 0.53P. P var? VB A (B = BD + 47deg 921, 9.30m,
A0V np:, 39.3", 175deg); SB 1.
IT Per dI = 0.06P. Min II 10.0, DII = 0.24P:, dII = 0.16P:.
VB (delta(m) = 1.7m, 12", 37deg).
The range of the combined
brightness is given.
IW Per SB 1. Min II 5.83.
IX Per The depth of Min II 0.02m.
VB A (B 10.6m, 5", 208deg).
IZ Per Min II 8.3.
KK Per See SU Per.
KP Per Beat phenomenon: P1 - see Table,
A1 = 0.0323m B; P2 = 0.1980855d, A2 = 0.0235M B; P3 =
= 0.2270986d, A3 = 0.0072M B.
KR Per Min II 11.1.
KS Per SB (Porb = 360.47d).
The main
component is a helium star. Besides the semiregular
variability (see Table), variations were noted with
P = 50 - 100 Min and delta(m) of several hundredths of a
magnitude. IR excess. Variable polarization (P - 1%).
KT Per Quasi-periodic oscillations during outbursts: P =
= 22.9s - 29.5s [5959], 82s, 90s, 147s [9791], delta(m)
up to ~ 0.01m.
KV Per [Fe/H] = - 0.96. P var. Max = 2428950.400 + 0.24942d*E
(JD2428950 - 29200); since JD2429500 -
see Table.
KW Per Min II 10.8. P var. Min = 2426295.450 + 0.931255d*E
(JD2423400 - 39500) [4009]; since JD
2440000 - See Table.
KY - LQ Per
See SU Per.
LR Per Very red. See SU Per.
LX Per mu alfa = +0.0065s, mu delta = -0.063". Min II 8.38m. .
DII = 0.05P.
Migrating distortion wave:
P = 475d [9792], delta(m) up to 0.04m.
MS Per Min II 12.1.
MX Per IR excess.
NP Per Min II 13.0.
NR Per P var. Max = 2416780 + 323.0d*E (JD2415750 -
24550); Max = 2435060 + 340.2d*E (JD243350 - 35400);
since JD2436700 - see Table.
NU Per A close pair, var
is the southern star.
OV Per D ~ 2h.
PP Per See SU Per.
PR Per See SU Per.
QR Per Red.
QU Per d = 0.03P.
QW Per Min II 14.7:.
QX Per Min II 16.1.
V345 - V347 Per
In the nebula NGC 1579.
V351 - V352 Per
See SU Per.
V354 - V356 Per
See SU Per.
V357 Per See SU Per. P = 0.21955d is possible.
V358 - V359 Per
See SU Per.
V360 Per See SU Per.
Other possible periods: 0.40036d, 0.40154d.
V361 Per See SU Per.
V363 Per Red.
V364 Per Min II 15.6, Max II 14.8.
V365 Per Min II 14.3:.
V376 Per P2 = 0.09165d, A2 = 0.016m; P1 - see Table,
A1 = 0.037m. A var.
V380 Per SB (Porb = 26d?). The epoch
of Min light is given.
V382 Per See SU Per.
V392 Per The southern
component of a very close pair.
V394 Per H2O maser.
V395 Per VB A (B 3.5", 90deg).
V396 Per In the
region of the open cluster alfa Per.
observations
are also satisfied by P ~ 1.678d. According
to [7586], P = 2.4928d or 1.6857d.
V397 Per ADS 2859 B (A = X Per; B 22.5", 12deg).
V398 Per IN type is also possible.
V403 Per See SU Per.
V409 Per Epoch of Min is given.
V423 Per ADS 2433 A (B 11.9m, 30.8", 99.2deg); SB.
Porb is given.
V424 Per See SU Per. IR excess.
V425 Per VB A(B 12.8m, 3.6", C 14.3m, 6.8"). See SU Per.
V428 Per According to [8639], type IS?
V432 Per Min II 11.6.
V434 Per Min II 14.9.
V436 Per Min II 5.74; Min II - Min I = 0.413P; D II = 0.03P.
V437 Per In the region of the open cluster NGC 744.
V438 Per See SU Per. VB (8.7m, 10.9m, 1".2, 26deg).
Min II 8.34. The range of combined brightness
variation is given. The bright component is
considered to be variable. This suggestion
needs verification.
V439 Per See SU Per.
V440 Per See SU Per. ADS 1820 A (B 14.5m, 8".3, 122deg).
V449 Per Min II 13.3.
V451 Per Min II 15.8.
V459 Per In the alpha Per cluster.
V461 Per See V459 Per.
V462 Per Min II 14.0.
V465 Per P2 = 0.030d is superimposed.
V466 Per Superposition of P1 = 5300d +- 250d, P2 = 475d +- 35d
(delta(m) = 1.1m), P3 = 0.26d (delta(m) = 0.5).
V468 Per P1 = 925s, P2 = 1022s. mu = 0".29, p = 170deg.
V469 Per Changes of line profiles with periods 0.150d, 0.188d,
0.304d, 0.476d, 0.608d, 1.88d [9814].
In 1978/1979 non-radial pulsations were observed:
P1 = 1.74d. P2 = 2.04d [4173, 4180].
V470 Per VB A (B 18.8m B, 1" - 2").
V471 Per The central star of the planetary nebula M 1 - 2 = VV8.
According to [9815, 9816], const.
bet Per Multiple system (Eclipsing pair = Algol AB; Algol C 4.7m,
Am, a = 0".10, Porb = 1.862a); Algol AB = ADS 2362 A
(B 12.7m, 57".5, 156deg, 1920). P var. P = 2.8673442d
(1784 - 1835); P = 2.8673012d (1835 - 1854); P = 2.8672775d
(1854 - 1901); P = 2.8672967d (1901 - 1913); P = 2.8672506d
(1913 - 1915) [6156]; Min I = 2424477.806 + 2.86730236d*E
(JD2420500 - 25000); Min = 2425917.203 + 2.86732697d*E
(JD2425000 - 277000); Min I = 2433194.454 + 2.86731667d*E
(JD2427700 - 33600); Min I = 2433928.4944 + 2.86732442d*E
(JD2433600 - 37000); Min I = 2437598.6766 + 2.86733732d*E
(JD2437000 - 42200); since JD2442200 - see Table.
Porb (Algol C) = 1.862a may be traced in the deviations;
a period of 32a may also be real. Depth of Min I var.
Variable polarization, changes in hydrogen line profiles,
sometimes emissions in the spectrum. Radio source with
frequent burst of different amplitude, faint X-ray source.
del Per Variable emission lambda 1650 A [6905]. Vr var, A = 16 km/s.
Per In the far IR range (lambda = 10 mkm) delta(m) > 1m. In
the far IR range (lambda = 10 mkm ) delta(m) > 1m; the
variability is related to mass loss.
omi Per VB A (B 8.4m, 0.96'', 29.7deg,1972). Possible superposition
of BCEP type oscilations.
ro Per A slower variation of the mean light is possible.
mu alfa = 0.0111s, mu delta = -0.102''.
fi Per SB 2. (Porb = 126.696d). V sin i = 450km/s. A var (P ~ Porb).
b Per SB 2. Depths of minima differ by 0.03m. Third body? ,
P = 701d. Radio source. In the region of the open cluster
NGC 1545.
R Phe P var. Max = 2405121 + 271.0d*E(JD2405000 - 11500);
Max = 2414570 + 266.26d*E(JD2414500 - 25500);
since JD2425500 - see Table.
T Phe P var. Max = 2411252 + 281.00d*E(JD2410000 - 30000);
since JD2430000 - see Table.
W Phe P var. Max = 2414960 + 328.65d*E(JD2414500 - 19500);
Max = 2424530 + 332.87d*E(JD2424500 - 30200);
since JD2436000 - see Table.
RS Phe P var?
RT Phe P = 208d?
RV Phe P var?; (k-b)2 = 0.06; delta(S) = 8:
SX Phe mu = 0.894", ro = 163.1deg. P var. Max = 2433923.9618 +
0.054964519d*E1 - 0.00337d sin 2pi (0.28503379*E1 + 0.074)
(JD2433900 - 36900); since JD2436900 - see Table.
There is a periodic term in the elements given in the Table:
-0.00325 sin 2pi (0.28503575*E2 - 0.107). According to
[9614] for epoch 1950.0 P0 = 0.054964509, P1 = 0.042772831,
Pb = 0.1928355; dP0/dt = -87*10**-13, dP1/dt = -174*10**-13,
dPb/dt = 2.46*10**-10. P1/P0 = 0.778; 0.8m <= A <= 0.3m;
0.2p <= M-m <= 0.4p. [Fe/H] = -0.6.
WW Phe Min II 12.7.
YZ Phe Min II 13.0.
AD Phe Min II 10.80. P var. Min I = 2436847.375 + 0.3799277*E
(JD2428650 - 36850); since JD2436850 see Table.
AE Phe Min II 8.19; 0.033p <= dI <= 0.05p; dII = 0.00. The
shape of the light curve varies with periods 55.9d and
95.3d [9615]. P var. Min I = 2440857.8140 + 0.36237459*E
(JD2438250 - 40870) [7388]; Min I = 2441969.57074 +
0.36237186d*E (JD2440870 - 42000) [9616]; Min I =
2442654.8201 + 0.3623741d*E (JD2441950 - 42660) [9533];
since JD2443700 - see Table.
AG Phe Min II 8.95. P var. Min I = 2440415.231 + 0.7553429d*E
(JD243800 - 40850); since JD2443750 - see Table.
AI Phe Min II 8.89; dI = 0.0035; Min II - Min I = 0.46p.
AU Phe Min II 13.0. According to [9517] the P value given in
the Table is wrong.
AX Phe mu = 0.234", p = 70deg. Multiperiodical: P i = 606.8s,
682.7s, 744.7s, 840.2s (A i ~ 0.01m).
gam Phe SB1 (P orb = 193.85d).
zet Phe VB A (B 7.0m, A7:, 0.46", 51.4deg, 1965.9; C 8.0m,
F7V, 6.4"). Total light range of A and B components is
given in the Table. Min II 4.22, MinII - MinI = 0.507p;
dII = 0.02p.
iot Phe VB A (B 12.7m, 7.7", 270deg).
ksi Phe VB A (B 12.1m, 13.2", 253deg). Epoch of MinI(v) is given
in the Table. A(v) = 0.13m.
ro Phe Frequency analysis results see also in [9619, 9620, 9621].
psi Phe SB.
R Pic P var. Max = 2413413 + 165.8d*E (JD2413000 - 23600);
since JD2423600 - see Table. Light curve (1923 -1953) [1054].
S Pic P var. Max = 2413595 + 424.7d*E (JD2405500 - 23000);
since JD2423000 - see Table. OH emission.
U Pic P var. Max = 2428103.565 + 0.44036450*E (JD2414000 -
29000) [0353]; since JD2438400 - see Table. (k - b)2 =
0.17; delta(S) = 3.
X Pic Min II 10.8
RR Pic Since 1965 periodic light variations were detected
with A(B) = 0.33m and elements Max = 2438815.380 +
0.14502545d*E. These variations are superimposed by
otHers with A(B) = 0.036m and period ~ 15.6 min or
15.4 min [9612]. There are also rapid oscillations
with periods in the range 20 - 40s [9613].
RT Pic Not seen only on one plate; defect?
RV Pic Min II 9.79.
SU Pic Min II 10.4.
del Pic Min II 4.83.
R Psc P var. Max = 2418070 + 344.14d*E (JD2397070 - 27700);
Max = 2432866 + 347.1d*E(JD2427300 - 33000) - see Table.
S Psc P var. Max = 2406665 + 405.6d*E (JD2398944 - 2407100);
Max = 2415930 + 402.6d*E (JD2407100 - 16500); Max =
2421295 + 413.7d*E (JD2416500 - 21500) - see Table.
U Psc P var. Max = 2417230 + 172.71d*E (JD2407720 - 18000);
Max = 2423840 + 174.3d*E (JD2418000 - 24000) [0001];
Max = 2424527 + 170.3d*E (JD2423000 - 26100) [0960];
Max = 2432514 + 174.05d*E (JD2425000 - 33000) [0001];
since JD2433000 - see Table.
V Psc mu alfa = 0.0112s, mu delta = -0.215".
W Psc P var. Max = 2412690 + 189.08d*E (JD2412692 - 27100) [1193];
since JD2435000 - see Table.
X Psc P var. Max = 2433474 + 357.3*E (JD24295000 - 38000); since
JD2438000 - see Table.
Y Psc P var. Min = 2410002.844 + 3.76582d*E (JD2410000 - 19700)
[9707]; Min = 2425495.522 + 3.765903d*E
(JD2423200 - 6300) [1072]; Min = 2430613.384 + 3.7658895d*E
(JD2427300 - 30620); Min = 2432865.357 + 3.7658405d*E
(JD2430620 - 32900); Min = 2435693.452 + 3.7657765d*E
(JD2432860 - 36600) [0001]; Min = 2441225.473 + 3.765859d*E
(JD2439000 - 42500) [6956]; Min = 2443142.29056 +
3.7658491d*E (JD2442500 - 44000) [8593]; since JD2444000 -
see Table.
RS Psc In the region of the galaxy NGC 251.
RT Psc Mean brightness varies with P2 = 533d. According to [8643]
30d <= P1 <= 70d.
RU Psc [Fe/H] = -1.65. P var. [0752, 9714] Max = 2415407.609 +
0.3903008d*E (JD2414400 - 15700); Max = 2416022.660 +
0.3902139d*E (JD2415700 - 16600); Max = 2417244.537 +
0.3902878d*E (JD2416600 - 19200); Max = 2419936.853 +
0.3903520d*E (JD2419200 - 22000); Max = 2425894.778 +
0.3903016d*E (JD2422000 - 26200); Max = 2426214.829 +
0.3903546d*E (JD2426200 - 27300); Max = 2427397.519: +
0.3902216d*E (JD2427300 - 28000); Max = 2428165.524 +
0.3903535d*E (JD2428000 - 29300); Max = 2429488.868: +
0.3904577d*E (JD2429300 - 600) [0752]. Max = 2430053.353 +
0.390202d*E (JD2430000 - 650); Max = 2430935.366 +
0.390354d*E (JD2430600 - 940); Max = 2431331.307 +
0.390457d*E (JD2430940 - 31350); Max = 2432119.417 +
0.390346d*E (JD2431350 - 32120); Max = 2433162.250 +
0.390283d*E (JD2432100 - 33200); Max = 2433905.311 +
0.390261d*E (JD2433200 - 33910); Max = 2433905.311 +
0.390321d*E (JD2433900 - 35430); Max = 2435429.502 +
0.390412d*E (JD2435420 - 35800); Max = 2435781.265 +
0.39027d*E (JD2435780 - 36130); Max = 2436501.361 +
0.39032d*E (JD2436130 - 36510); Max = 2436534.190 +
0.39043d*E (JD2436500 - 36850); Max = 2436845.351 +
0.39025d*E (JD2436840 - 37200); Max = 2437181.358 +
0.39031d*E (JD2437180 - 37610); Max = 2437994.329 +
0.39026d*E (JD2437610 - 38000); [0001]. Max = 2438303.950 +
0.39040d*E (JD2438000 - 38400) [3879]. Max = 2438375.409 +
0.39027d*E (JD2438370 - 38650) [0001]. Max = 2439435.2421 +
0.390385d*E (JD2438650 - 39500) [9713]. Max = 2439435.242 +
0.390313d*E (JD2439430 - 39800); Max =2439771.3049 +
0.39046d*E (JD2439770 - 40140) [0001]. Since JD2440140 -
see Table. According to [3569] A var with P = 28.8d.
RV Psc Min II 12.0.
RY Psc (k-b)2 = 0.03, delta(S) = 7. P var. Max = 2419677.268 +
0.52971027d*E (JD2414000 - 22000); Max = 2425148.192 +
0.52972643d*E (JD2422000 - 25500) [1337]; Max =
2425508.390 + 0.5297291d*E (JD2425500 - 40000);
Max = 2441538.476 + 0.52972911d*E (JD2441000 - 41650)
[7984]; since JD2442660 - see Table.
RZ Psc Algol-like.
SS Psc (k-b)2 = 0.19; delta(S) = 2. Blazhko effect: -0.04d <= O-C <=
+ 0.04d; Min(O-C) = 2437520 + 136d*E [9731].
SU Psc Min II 11.3.
SW Psc P var. Max = 2425177.298 + 0.5212844d*E (JD2419670 -
25200) [4191]; Max = 2425177.256 + 0.5212642d*E
(JD2425170 - 38000) [3506]. Since JD2438600 - see Table.
THere is a periodic term in the elements given in the
Table: + 0.0132d sin 5.440deg (E + 2). Blazhko effect (Pi = 34.5d).
SX Psc P var. Min = 2427811.357 + 0.825882d*E (JD2425580 - 36000)
[1218]; Min = 2437202.453 + 0.825877d*E (JD2436000 - 39900)
[0001]; since JD2439800 - see Table.
SZ Psc Min II 7.38. P var.
There is a square
term in the elements given in the Table: -0.113d*10**-6*E**2.
TY Psc Porb = 0.080d [9735].
The cycle of supermaxima is 370d [9675].
UU Psc VB A (B 7.60m, F4V, 11.5", 148deg, 1966.9). Min II 6.04;
Min II - Min I = 0.55P.
Elliptical orbit and
rotation of the line of apsides are possible.
UV Psc Min II 9.54. P var. Min I = 2424134.574 + 0.8610475d*E
(JD2414600 - 24150) [0001]; Min I = 2428038.555 +
+ 0.861046d*E (JD2424150 - 36700) [2924];
since JD2436700 - see Table.
The shape of the light
curve varies.
UW Psc Min II 11.0:.
UZ Psc SB 1 (Porb > 1 yr [5751]).
VZ Psc Mu = 0.43", P = 65deg. Min II 10.43.
WW Psc VB A (B 13.1m, 31").
WX Psc OH, H2O, SiO maser.
ZZ Psc P1 = 612s, P2 = 816s [7476].
Nonradial modes [8467].
AG Psc P (Vr) = 0.055d.
AH Psc The star was seen in 1854 - 60; since
1862 it was not observed.
AO Psc Epoch
of Max brightness is given. Light variations with
Porb = 0.1496263d are superimposed by variations with
P = 858.6861s and twice smaller amplitude (Max =
= 2444815.00276 + 0.009938496d*E; M-m = 0.54P), and
also by still smaller oscillations with P = 805.2059s
(Max = 2444815.00294 + 0.009319513d*E). The last pe-
riod is the X-ray impulse period which is equal to
the period of rotation of the compact object (probably
a white dwarf).
R PsA P var. Max = 2417385 + 293.00d*E (JD2405000 - 26000);
Max = 2432896 + 291.50d*E (JD2426000 - 38000);
since JD2438000 - see Table.
S PsA P var. Max = 2417853 + 271.0d*E (JD2411000 - 18000);
Max = 2426880 + 273.6d (JD2418000 - 27000); Max =
= 2434714 + 270.3d (JD2427000 - 35000); since
JD2434000 - see Table.
X PsA Min II 14.2.
RW PsA Min II 11.63.
TX PsA VB B (A 13.0m pg; B 37", 131deg); mu = 0.22", p = 117deg.
pi PsA SB (Porb = 178.3177d [5769]).
R Pup In the region of
the open cluster NGC 2439.
U Pup P var. Max = 2415090 + 314.26d*E (JD2408000 - 22800);
since JD2422800 - see Table.
V Pup VB A (B 10.0m, 7", 0, 70deg; C 11.0m, 19.0", 48deg).
Min II 4.82. P var. IO - CI < 0.02d.
W Pup P var. Max = 2420990 + 120.68d*E (JD2412500 -
23600); Max = 2424725 + 119.9d*E (JD2423600 -
26300); Max = 2432200 + 120.68d*E (JD2426300 -
40800); since JD2440800 - see
Table.
X Pup P var. Max = 2414889.8 + 25.939d*E (JD2408800 -
16000); Max = 2435188.76 + 25.9610d*E (JD
2419000 - 35190) [2392]; Max = 2436279.50 + 25.97d*E
(2435190 - 38000) [0001]; since JD2438000 -
see Table.
Z Pup OH, H2O, SiO emission.
P var. Max = 2424256 + 513.90d*E (JD2413900 - 24500);
since JD2424500 - see Table.
RS Pup Surrounded by the reflecting nebulosity with a
radius of 1.4' [9634].
P var. Max = 2419186.3 + 41.337d*E (JD2414000 -
24000) [2049]; Max = 2427083.613 + 41.414d*E
(JD2425800 - 28300) [2440]; Max = 2434823.23 +
+ 41.38535d*E (JD2433750 - 34900) [9636];
since JD2435700 - see Table.
RW Pup P var. Max = 2430175 + 332.5d*E (JD2424500 - 30200)
[0001]; since JD2435800 - see
Table.
RX Pup Light curve
(1890 - 1925) [1265].
Mira
type component light variations are observed in the
infrared region of spectrum: Max = 2444530 + 580d*E,
3.99m - 6.00m J, M - m = 0.50P [9518].
ST Pup [A/H] = -0.9.
The light curve shape And the period va-
ry strongly: 0.10P < M - m < 0.30P; 17.4d < P < 19.19d.
P = 19.188d (JD2415000 - 17000); 18.949d (JD
2417000 - 18000), 18.8065d (JD2418000 - 19000),
18.721d (JD2419000 - 20000), 18.714d (JD2420000 -
21000), 18.717d (JD2421000 - 22000), 18.6175d (JD
2422000 - 23000), 18.678d (JD2423000 - 24000),
18.735d (JD2424000 - 25000), 18.796d (JD2425000 -
26000), 18.817d (JD2426000 - 27000) [1266]. Max =
= 2427779.6 + 18.846d*E (JD2427000 - 28000) [1266];
Max = 2428893.9 + 18.885d*E (JD2428000 - 29000)
[0016]; Max = 2429697.51 + 19.188d*E (JD2429000 -
30000) [1266]. P = 19.142d (JD2430000 - 31000),
19.145d (JD2431000 - 32000) [1266].
Max = 2435395.430 + 18.559d*E (JD2435160 - 500)
[6006]; Max = 2435617.45 + 18.8864d*E (JD2435500 -
5620) [2309]; Max = 243957.3 + 17.4d*E (JD2438700 -
39600) [6611]; since JD2444000 -
see Table.
SV Pup P var. Max = 2419010 + 166.6d*E (JD2413660 - 18000);
Max = 2423090 + 169.8d*E (JD2418000 - 23100);
Max = 2426782 + 167.8d*E (JD2423100 - 27500);
since JD2427500 - see Table.
SW Pup Min II 9.1; d = 0.029P.
TT Pup Min II 13.6.
TY Pup Min II 8.87.
UZ Pup Min II 10.0.
VV Pup mu = 0.100", P = 165.0deg.
The epoch of light maximum is given. The mean
brightness varies by 2 - 3m. Intervals of active light
variation with amplitude up to 2m during maximal mean
brightness are observed. During low activity inter-
vals when amplitude is about 0.3m mean brightness is
minimal; during this time the ellipsoidal light varia-
tions of the system are observed in the range 15.1m -
15.3m J with the elements Min = 2427889.6509 +
+ 0.0697468256d*E [9644]. The white dwarf rotation
period is equal to the orbital period. There are
flickerings. Spectrum description [9472, 9645].
VW Pup P var. Max = 2425184.67 + 4.28405d*E (JD2422660 -
25600) [0973]; Max = 2435554.86 + 4.28519d*E (JD
2425600 - 35600) [2309]; since JD2435500 -
see Table.
VX Pup P1 = 2.1389d (A1 = 0.29m); A0 = 0.31m; P1/P0 = 0.71042.
VY Pup The depth of Min II 0.04m.
VZ Pup [A/H] = -0.3. P var. Max = 2434864.90 + 23.1640d*E
(JD2426700 - 35300) [2309]; since
JD2435300 - see Table.
WW Pup P var. Max = 2424497.73 + 5.5159d*E (JD2423520 -
26000) [0973]; since JD2426000 -
see Table.
WX Pup P var. Max = 2435042.184 + 8.93825d*E (JD2422000 -
35100) [2431]; since JD2435000 -
see Table.
WZ Pup P var. Max = 2427861.33 + 5.02657d*E (JD2421100 -
29400) [2392]; since JD2429400 -
see Table.
XX Pup P var. Max = 2426338.503 + 0.51719805d*E (JD
2426300 - 39500) [3572]; since JD2441700 -
see Table.
(k - b)2 = 0.07. The
spectral type according to CA II is given.
XY Pup Min II 9.4; d = 0.042P.
XZ Pup Min II 7.90. P var. Min I = 2440629.7969 + 2.192383d*E
(JD2425850 - 41700) [0099]; since JD
2441700 - see Table.
YY Pup The depth of Min II 0.05m.
AE Pup In the region of
the open cluster CR 173.
AF Pup Min II 13.5.
AG Pup Min II 10.9.
AH Pup See YY Pup.
AN Pup Min II 10.7.
AQ Pup VB A (B 11.13m, < 15"; C 12.83m, < 15"). [A/H] = -0.1.
The
range of the variation of combined light is given.
P var. Max = 2429734.59 + 29.931d*E (JD2427500 -
33000) [3474]; Max = 2433296.2 + 30.018d*E (JD
2433000 - 35850) [2474]; Max = 2436625.9 + 29.8568d*E
(JD2435850 - 36700) [3601]; Max = 2441760.63 +
+ 30.032d*E (JD2436600 - 42700) [9671];
since JD2443400 - see Table.
AR Pup The mean
brightness varies with P = 1200d.
AS Pup In the region of
the open cluster NGC 2546. P var. Max = 2416110 +
+ 331.4d*E (JD2415460 - 26000); since
JD2426000 - see Table.
AT Pup In the region of
the open cluster NGC 2546.
P var. Max = 2426758.205 + 6.6648d*E (JD2426700 -
35600) [2202]; since JD2435600 -
see Table.
AU Pup Min II 9.28. P var. Min I = 2428111.304 + 1.126418d*E
(JD2414700 - 28200) [0007]; since
JD2439000 - see Table.
AV Pup Min II 11.0.
AW Pup VB A (B 11.7m, 3.7", 258deg).
Period probably must be doubled.
AY Pup Min II 12.5.
AZ Pup Min II 10.1.
BB Pup (k - b)2 = 0.24; delta(S) = 3.
BH - BK Pup
See AE Pup.
BL Pup Min II 14.2.
BN Pup In the region of the
open cluster NGC 2533.
BP Pup Min II 12.3.
BQ Pup The
shape of the light curve possibly varies.
BR Pup Min II 12.9.
BT Pup Min II 14.5. In the
region of the open cluster NGC 2482.
BU Pup Min II 13.9. In the
region of the open cluster NGC 2447.
BW Pup The depth of Min II 0.15m.
BX Pup In the region of
the open cluster NGC 2482.
CE Pup P var? [7934].
CH Pup P var. Max = 2428465 + 491.0d*E (JD2428400 - 37300);
since JD2437300 - see Table.
CO Pup P var? The epoch of light
minimum is given.
CP Pup In 1981 the radius of the
shell expanding with Vexp = 710 km/s was equal to
7" [9689, 9559].
CX Pup d = 0.05P.
CY Pup d = 0.01P:; Min II 13.0.
CZ Pup Min II 13.1.
DD Pup Min II 14.6; Min II - Min I = 0.572P.
DE Pup Min II 12.9.
DF Pup Min II 12.8.
DK Pup Min II 13.0.
DM Pup Min II 13.7; Min II - Min I = 0.62P.
DN Pup Min II 13.5.
DO Pup Min II 13.3.
DR Pup Min II 13.3:.
DS Pup Min II 13.4.
DT Pup Min II 14.3.
EK Pup VB A (B 15", 270deg). P var? Max = 2427747.89 +
+ 2.62587d*E (JD2425500 - 29500) [1343];
since JD2434500 - see Table.
EL Pup P > 1.3d? See GI Pup.
EN Pup Min II 11.4.
EQ Pup Min II 10.9.
ES Pup According to [0412], Max = 2430377 + 187d*E.
The
elements given in the Table are valid in the interval
JD2425600 - 29700.
EU Pup Min II 14.8.
FK Pup A var (P2 = 3000d).
Strong SiC2 bands in the spectrum.
FM Pup Min II 14.2.
GG Pup S5/5.
GH Pup VB A (B 10", 195deg; C 16", 280deg; D 14", 315deg). P var.
Max = 2425450 + 800d*E (JD2425300 - 28000);
since JD2428700 - see Table.
Very red.
GI Pup In the region of
the open cluster NGC 2437.
GK Pup See GI Pup.
GN Pup VB A (B 16.5m, 10", 80deg).
GP Pup Min II 13.5.
GU Pup Min II 12.2.
GX Pup Min II 13.9. See AE Pup.
GY Pup Min II 12.3.
GZ Pup Min II 12.1.
HH Pup (k - b)2 = 0.14, delta(S) = 1.
HI Pup Min II 11.0. See AE Pup.
HK Pup P var. Max = 2425925.732 + 0.7342532d*E
(JD2425300 - 36600) [4127]; since JD
2436600 - see Table.
HM Pup THere is a shallow Min II.
HP Pup P var?
HW Pup P var? Max = 2429756.28 + 13.4532d*E (JD2427100 -
33000) [3551]; since JD2433000 -
see Table.
KQ Pup In the open cluster NGC
2422. SB 2 (Porb = 9752d [3985]).
KT Pup Min II 13.4.
KW Pup Min II 11.8.
KX Pup Min II 13.04; 0.435P (1930) < Min II - Min I < 0.56P (1973)
[3474, 8094]; e = 0.15. Apsi-
dal motion.
KY Pup Min II 11.1.
LN Pup Min II 12.9; Min II - Min I = 0.533P.
LO Pup Min II 13.9.
LP Pup d = 0.03P:.
LT Pup Min II 12.6.
MN Pup Min II 13.2.
MQ Pup Min II 9.39.
MT Pup RCB?
MW Pup Min II 9.2.
NO Pup VB A [BC 7.19m V, 8.1". 124deg (delta(M) = 0.0m, 0.20", 275deg,
1976)]. Min II 6.66; Min II - Min I = 0.582P; e = 0.123.
NQ Pup S 4.5/2-.
NW Pup Porb = 1d.
NX Pup Connec-
ted with a cometary nebula.
OR Pup In the region of
the open cluster NGC 2467.
OS Pup VB A (B 6.10m, 67.4").
In the region of the open cluster C 0812-362.
OU Pup In the region of
the open cluster IC 2391.
OX Pup In the region of the
open cluster NGC 2451.
PS Pup The depth of Min II 0.028m.
PT Pup P2 = 0.168377d. A (lambda 1550) = 0.043m; 0.015m < A(B) <
< 0.035m.
PU Pup VB (5.2m, 5.6m; 0.11", 43.6deg, 1927). Min II 4.74.
PV Pup VB B (A 6.1m; B 16.9", 340deg; C 10.5m, 100.4", 228deg).
Min II 7.31; DII 0.10P; Min II - Min I = 0.47P.
The light
curve shape in Max And Min II varies. The deviations
DB from the mean curve vary from -0.06m to +0.03m
with the elements: Max (Idelta(b)I) = 2440000.027458 +
+ 1.92207d*E or Max (Idelta(b)I) = 2440000.219470 +
+ 0.48003d*E.
PW Pup Min II 9.54; d = 0.095P. See R Pup.
QS Pup 0.008m <= A(u) <= 0.015m.
QT Pup Probably a
member of the open cluster NGC 2477.
QU Pup P2 = 0.1680d or 0.2019d; 0.010m <= A(u) <= 0.040m.
QV Pup May be a
member of the open cluster NGC 2489.
RO Pup VB A (B 13.7m, 29.6", 15deg). [Fe/H] = +0.13. P var.
Max = 2435552.807 + 0.14088141d*E (JD2413900 -
37500) [9756]; Max = 2439887.843 + 0.14088141d*E
(JD2439800 - 43700); since JD2444000 -
see Table.
L2 Pup VB A (B 11.5m, 62", 214deg); mu = 0.34", P=18deg. H2O, SiO
maser.
S Pyx P var. Max = 2411770 + 206.60d*E (JD2405500 - 23700);
Max = 2423765 + 207.0d*E (JD2423700 - 29600);
since JD2429600 - see Table.
T Pyx Previous outbursts were obser-
ved in 1890, 1902, 1920, 1944.
RR Pyx A close companion 14.5m.
RZ Pyx Min II 9.69.
SU Pyx d = 0.016P.
TT Pyx P = 3.031556d?
TV Pyx Depth of Min II 0.05m.
TX Pyx Min II 9.8.
TY Pyx Min II 7.48.
TZ Pyx Min II 11.1.
UZ Pyx VB A (B 7.61m, 110", 180deg).
VV Pyx VB A (B 8.58m, 0.3").
Range of the variation of combined
light is given. Min II 7.03; DII = 0.08P; Min II - Min I =
= 0.48P. Min II = 2444622.86709 + 4.5961766d*E.
Apsidal motion (P = 3200 yr.).
VW Pyx The nucleus
of the planetary nebula K 1-2.
The range
of the variations of combined light: 15.7 - 17.4 pg.
The value of P close to
that found by bond [9767] And the epoch of Max bright-
ness are given in the Table.
R Ret P var. Max = 2403013 + 280.0d*E (JD2403000 - 13900);
Max = 2423317 + 276.68d*E (JD2413900 - 25300);
Max = 2430008 + 279.7d*E (JD2425200 - 30020);
since JD2430000 - see Table.
T Ret Mean brightness
varies with P = 200d.
X Ret (k - b)2 = 0.09. P var. Max = 2427425.47 + 0.4920d*E
[0357]; Max = 2434334.611 + 0.492011d*E (JD2434300 -
600) [0080]; since JD2434600 -
see Table.
The shape of the light curve varies. Blazhko effect:
Pi >= 45d; 0.13P <= M - m <= 0.23P [0080].
R Sge P var (70.07d <= P <= 71.24d [9769].
Period variation study [0767].
The elements given in the
Table are valid since JD2434000.
The mean brightness vari-
ES: Min = 2414402 + 1112.d*E [1357].
S Sge SB1 (Porb = 675d [1358]). P var. Max = 2409863.32 +
+ 8.381968d*E (JD2406600 - 18000); since
JD2418000 - see Table.
U Sge VB A (B 9.6m, 92.0", 318deg). Min II 6.71; 0.014P <= dI <=
0.024P. In the region of the open cluster
Col 399. Not a member of the cluster. P var [6224,
8608].
Mean elements are given in the Table representing
epochs of Min within +-0.008P.
The shape of the light curve varies.
V Sge VB A (B 13.9m, 9.7", 267deg); SB 2 (K1 = 320 km/s,
K2 = 85 km/s). P var? The depth of eclipses
varies from 0.6m to 1.3m. The mean brightness outside
eclipses varies. There are also flares with amplitu-
des up to 3m and small light variations with a time
scale of minutes, dozens of minutes and a few days.
spectrum description [3593, 9472].
X Sge VB A (B 13.18m, 6", 248deg).
Z Sge V1 (NGC 6838, M71).
Globular cluster member. P var. Max = 2437870 + 175.3d*E
(JD2437000 - 38700); since JD2438700 -
see Table.
RS Sge The mean brightnese
varies: Max = 2435999 + 1124d*E [8104].
Two Algol-like light weakenings were also
observed: JD2444837.22, 2444865.17 [9727].
RW Sge P var. according to [1363] Max = 2424289 +
+ 429d*E. Since JD2434000 - see
Table.
RZ Sge Porb ~ 97m [9771].
Mean cycle is given according to [9785]. Supermaxima
are repeated with the cycle 266d. The period of super-
humps decreases from 101.3m till 100.8m.
SY Sge Min II 10.7. P var.
Elements given in the
Table are valid in the interval JD2425800 - 38300.
TU Sge d = 0.035P.
TX Sge P var. Max = 2425002 + 155.0d*E (JD2414900 - 25100);
since JD2425000 - see Table.
UU Sge VB A (B 16.5m B, 4", 90deg).
The nucleus of the planetary nebula Abell 63.
Min II 14.41; d = 0.019P.
The range of the combined light variation is
given. The actual depth of Min I is about 4.3m.
Large reflection effect.
UZ Sge Min II 11.6:. P var. Min I = 2429961.231 + 2.215750d*E
(JD2429000 - 41600); since JD2441600 -
see Table.
VZ Sge VB A (B 12m, 28.2", 206deg).
WY Sge Nova Sge 1783 (Max JD2372494:). Min I = 2445137.8993 +
+ 0.1536342d*E; D = 0.16P.
Brightness outside eclipses is usual-
ly ~ 18.7m, the depth of the eclipses is ~ 1.5 - 2m. At
present outbursts by 1.6m are sometimes observed si-
milar to the UG type variable outbursts, as well as
rapid flickering of light [9708].
WZ Sge Nova Sge 1913, 1946, 1978. VB A (B 15.76m B, 7",
280deg).
Really it is not a nova. Three outbursts were registe-
red up to day: JD2420094, 32001, 43844 [9710, 9711].
There are superhumps on the light curve du-
ring the outburst with 0.057250d >= P >= 0.05714d (A=0.3m V)
[9710, 9776].
THere are light variations between
the outbursts (A = 0.14m - 0.3m). During some of light
weakenings Algol-like eclipses are observed (A =
= 0.2m) with the elements: Min I = 2437547.72845 +
+ 0.0566878455d*E [9774]; D = 0.04P. d = 0.02P.
THere are also rapid light oscillations (A <=
<= 0.01m). The periods of these oscillations before the
1978 outburst were 28.98s and 27.87s [9774], but af-
ter this outburst - 28.95963s [9775]. According to
[9777], in 1976 - 78 these oscillations were represen-
ted by the elements: Max = 2443311.790250 +
+ 0.00032254826d*E + 9.8d*10**-16*E**2.
XY Sge According to [3705] the spectrum is earlier than M0.
AG Sge P = 117d?
BR Sge d = 0.030P.
CP Sge Min II 13.3.
CU Sge Min II 11.3.
CW Sge Min II 11.7. P var?
The shape of the light curve varies.
CZ Sge Min II 15.2.
DH Sge The shape of the
light curve varies (1.1m <= A <= 1.7m).
P var. Max = 2427612.509 + 0.4695844D*E (JD2427600 -
38800) [4027]; since JD2438800 -
see Table.
Blazhko effect disappeared after the period
change (A = 1.1m).
DI Sge P var. Max = 2427929 + 203.0d*E (JD2427500 - 30200)
[2641]; since JD2437100 - see
Table.
DK Sge Min II 13.0.
DL Sge Min II 11.5.
DM Sge Min II 11.6.
DP Sge P var. Max = 2427985.464 + 0.4883395d*E (JD
2427985 - 33000); Max = 2432855.191 + 0.4883339d*E
(JD2433000 - 40775); since JD2440775 -
see Table.
DQ Sge Min II 14.8.
DS Sge Min II 16.0:.
DT Sge d = 0.05P:.
EH Sge VB A (B 15.6m).
EI Sge Min II 14.6.
ER Sge P var. Max = 2430515.460 + 0.4184209d*E (JD
2427000 - 38400); Max = 2438443.388 + 0.4184356d*E
(JD2438400 - 41800); since JD2441800 -
see Table.
FF Sge d = 0.03P; Min II 13.0.
FG Sge VB A (B 14.2m, 8", 100deg).
The central star of the planetry nebula PK 60deg
(diameter 36", the age about 6000 years). The bright-
ness of the star steadily increased from 13.6 pg in
1894 to the maximum in 1967, and then is steadily
decreasing. In 1982 it was 11.0 B. In 1967 the strong
absorption lines of rare earth elements appeared in
the spectrum. The spectral class steadily becomes
later. The signes of new planetary nebula ejection we-
re observed. In 1962 the star entered the instability
strip in the Mv, B-V diagram and began to pulsate
with a small amplitude and increasing period: Min(V) =
= 2442629 + 59.83d*E + 1.126d*E**2 (JD2442600 - 44530).
In twenty years the period increased from 50d to 134d,
the amplitude of pulsations changed from 0.2mV to
0.5mV; now it decreased again to 0.2mV, and the pe-
riod is only 90d [9780].
FH Sge Min II 13.5.
FL Sge There is a close companion 14m. In the
minimum probably fainter than 15.9m.
FO Sge P var. Max = 2427578.0 + 67.8d*E (JD2427570 - 28120);
Max = 2428134.4 + 72.7d*E (JD2428120 - 30150);
since JD2430150 - see Table.
FP Sge Min II 14.9. P = 0.32100275d?
FT Sge P.K.55 - 1deg 2. Not a pla-
netary nebula.
FU Sge Min II 15.8.
FX Sge In the region of the
globular cluster M71 (NGC 6838).
GI Sge Red.
GN Sge Min II 10.6.
GP Sge Red.
GY Sge P var. Max = 2431264.49 + 51.497d*E (JD2429490 -
34900) [7199]; Max = 2433787.42 + 51.5991d*E (JD
2433600 - 37280), Max = 437911.04 + 51.2594d*E
(JD2437280 - 40510) [6172]; since
JD2444450 - see Table.
HH Sge The cycles
23 - 26d and 300d are observed.
HM Sge VB A (B 14.20m, 10", 182deg).
The brightness increased
from 17.2m up to 11.3m pg in the interval JD2442280 -
42650. Then the light variations in the infrared region
appeared with P = 550d [9721, 9783] and A(K) = 1.5m.
Radio and X-ray source.
IR Sge SF star in a close pair.
LN Sge See IR Sge.
MV Sge Possible mem-
ber of the globular cluster Palomar 10.
MZ Sge See MV Sge.
PT Sge P component of a close
pair.
del Sge VB A (B, A = 0.04", P = 7 yr); SB 2 (Porb = 3725d [9789]).
The last superior conjunction of the B-star
and its atmospHeric eclipse was in March - April
1980 [9726].
R Sgr P var. Max = 2405776 + 271.0d*E (JD2399500 -
2407500); Max = 2407115 + 264.2d*E (JD2407100 -
9500); Max = 2418125 + 269.65d*E (JD2409500 -
19500); Max = 2433137 + 267.90d*E (JD2419500 -
36000); since JD2436000 - see
Table.
S Sgr P var. Max = 2401029 + 230.6d*E (JD2401000 - 10000);
Max = 2411638 + 229.2d*E (JD2410000 - 19500);
Max = 2422222 + 232.81d*E (JD2419500 - 27000);
since JD2427000 - see Table.
T Sgr Companion F3IV (ro < 0.8"). P var. Max =
= 2409013 + 385.1d*E (JD2401500 - 10500); Max =
= 2414582 + 399.0d*E (JD2413000 - 17500); Max =
= 2424363 + 387.9d*E (JD2417500 - 25500);
since JD2425500 - see Table.
S 5/6-e.
There are Te lines and a very strong
Li lambda 6708 line in the spectrum.
U Sgr The member of the open
cluster M25 (IC 4725).
P var. Max = 2416628.046 + 6.744925d*E (JD2404480 -
30115) [0765]; since JD2430115 -
see Table. [A/H] = 0.1.
W Sgr VB A (A 9.2m, 0.116", 153.3deg, 1976.477; B 13.5m, 33.4",
233deg; C 13.5m, 47.9", 101deg). P var. Max = 2403198.39 +
+ 7.594695d*E (JD2403100 - 34500); since
JD2434500 - see Table.
X Sgr P var. Max = 2410006.22 + 7.01206d*E (JD2403000 -
17000); Max = 2424248.11 + 7.01245d*E (JD2417000 -
34500); since JD2434500 - see
Table.
Y Sgr In the region of
the open cluster M25 (IC 4725).
RR Sgr P var. Max = 2410008 + 336.0d*E (JD2410000 - 17100)
[9794]; Max = 2422755 + 332.73d*E (JD2422700 -
32100) [0960]; since JD2432100 -
see Table. OH, H2O emission.
RS Sgr VB A (B 9.65m V, 39.0", 86deg). Min II 6.28.
RT Sgr P var. Max = 2412759 + 303.1d*E (JD2412700 - 8300)
[0960]; Max = 2425588 + 308.8d*E (JD2422800 - 26700);
Max = 2428034 + 303.8d*E (JD2426700 - 33500);
since JD2433500 - see Table.
RU Sgr P var. Max = 2413062 + 242.3d*E (JD2410150 - 16700)
[0960]; Max = 2423670 + 242.3d*E (JD2422500 -
24500); Max = 2428200 + 237.6d*E (JD2424500 -
28800); since JD2428800 - see
Table.
RV Sgr P var. Max = 2411206 + 319.3d*E (JD2410200 - 17000)
[0960]; Max = 2429032 + 321.3d*E (JD2422600 -
29500); since JD2429500 - see
Table.
RW Sgr P var. Max = 2413798 + 189.0d*E (JD2413700 - 23000);
Max = 2431998 + 190.87d*E (JD2423000 - 33500);
since JD2433500 - see Table.
RX Sgr P var. Max = 2417730 + 330.3d*E (JD2413000 - 18500);
Max = 2420122 + 346d*E (JD2418500 - 20150); Max =
= 2420122 + 323d*E (JD2420100 - 22200); Max =
= 2424120 + 345d*E (JD2422200 - 24200); Max =
= 2428785 + 332.2d*E (JD2424000 - 31500);
since JD2431500 - see Table.
RY Sgr VB A (B 15.69m, 12").
THere are pulsational light variations (0.1m < A < 1.5m)
with the elements: Max = 2433670 + 38.6056d*E -
- 78d*10**-5*E**2.
light curve [9798, 9799]; spectrum
description [6261].
ST Sgr S 6/3-e.
SU Sgr VB A (B 13.5m, 1.0", 240deg, 1932.45).
earlier P = 88d was observed [0017].
SV Sgr In the nebula M8 (NGC 6523).
SW Sgr P var. Max = 2416338 + 290.3d*E (JD2414000 - 16500);
Max = 2428507 + 288.5d*E (JD2422500 - 29000);
Max = 2429088 + 293.5d*E (JD2429000 - 33000);
since JD2433000 - see Table.
SX Sgr Min II 9.62; d = 0.05P. P var. Min I = 2429114.249 +
+ 4.15395762d*E (JD2410000 - 29150) [0007];
since JD2429000 - see Table.
SY Sgr In the region of the nebula
S 188.
SZ Sgr VB A (B 12.5m V, 2.0", 212deg.)
VV Sgr In the region of
the open cluster NGC 6494.
OH, H2O emission.
VX Sgr P var; 1m <= A <= 6m. SIO, H2O, OH maser.
Light curve (1935-1969) [6615].
VY Sgr [A/H] = 0.5.
WX Sgr VB A (B 12.5m, 0.4", 88deg). P var. Min = 2419317.259 +
+ 2.129095d*E (JD2419300 - 24700) [0457]; Min =
= 2424729.418 + 2.129113d*E (JD2424700 - 39700)
[0279]; since JD2440000 - see
Table.
WY Sgr Min II 10.3.
WZ Sgr The member of the open
cluster C 1814-190. [A/H] = 0.4.
XX Sgr P var. Max = 2419189.730 + 6.424264d*E (JD2419100 -
30100) [0637]; since JD2435000 -
See Table.
XZ Sgr Min II 8.95; d = 0.022P. P var. Min I = 2420311.519 +
+ 3.275537d*E (JD2420300 - 28000) [1604]; Min I =
= 2436440.137 + 3.27549d*E (JD2428000 - 37500)
[2516]; Min I = 2441150.348 + 3.2755357d*E (JD
2437500 - 41500) [7084]; since JD2441500 -
see Table.
YY Sgr Min II 10.64; Min II = 2433075.8296 + 2.628463d*E
[2302]. Apsidal motion period is about 300 years.
AL Sgr P var. Max = 2425792 + 79.07d*E (JD2421000 - 26000);
since JD2426000 - see Table.
AN Sgr P var. Max = 2425720 + 339.62d*E (JD2415000 - 26000);
Max = 2428360 + 330.0d*E (JD2426000 - 28500);
since JD2428500 - see Table.
AP Sgr SB? [9004].
AR Sgr There is A
square term in the elements: -[0.0031d (E-30)**2 + 8.8d].
AS Sgr Planetary nebula HB 6 =
= 7 + 1deg 1.
AU Sgr In the region of the open cluster and the
diffuse nebula NGC 6514 (M20).
AV Sgr In the region of the open cluster NGC
6546. Not a member of the cluster.
[A/H] = 0.4. P var. Max = 2429083.30 + 15.4093d*E
(JD2421400 - 39100); since JD2439100 -
see Table.
AW Sgr VB A (B 16m, 15", 97deg).
In the region of the open cluster NGC 6546.
AY Sgr [A/H] = 0.2.
BB Sgr VB A (B = V4088 Sgr, 7.49m - 7.87m, 93.5", 102deg).
In the region of
the open cluster Cr 394.
BE Sgr A var (0.6m <= A <= 1.1m).
BM Sgr P var.
BN Sgr Min II 9.37; d = 0.04P:.
Soft X-ray source. P var [1600].
BQ Sgr d = 0.017P. P var. Min = 2412592.7905 + 8.01964d*E
(JD2412590 - 22220) [1696]; since JD
2422220 - see Table.
CC Sgr In the region of the
globular cluster NGC 6723.
CD Sgr See CC Sgr. P var. Max = 2416247 + 266.62d*E
(JD2411000 - 23000); since JD2423000 -
see Table.
CE Sgr see CC Sgr.
SF component of a close
double.
CF Sgr See CC Sgr.
P var. Max = 2415632.81 + 0.570026d*E (JD2411000 -
23800) [1616]; since JD2423900 -
see Table.
CG Sgr see CC Sgr.
DH Sgr In the region of the
globular cluster NGC 6809 (M55).
DI - DK Sgr
See DH Sgr.
DM Sgr See DH Sgr.
DO - DP Sgr
See DH Sgr.
DR - DS Sgr
See DH Sgr.
DV Sgr d = 0.044P.
EG Sgr d = 0.010P.
FV Sgr P var. Max = 2424010 + 269.5d*E (JD2424000 - 27500)
[0251]; since JD2427500 - see
Table.
GG Sgr P var. Max = 2413840 + 286.5d*E (JD2413800 - 24000);
since JD2424000 - see Table.
GK Sgr According to [5869] -
eclipsing.
GU Sgr There are
also light variations with = 37.5d, 0.4m <= A(V) <=
1.5m [6273].
HH Sgr VB (ro = 0.1').
IR Sgr VB B (A 13.6m; B 10", 220deg).
KO Sgr Similar to UG. It is possible
that the observations in Min brightness refer to a
companion.
LZ Sgr VB A (B 16m, 7", 30deg).
MV Sgr Very hot hydrogen deficient extreme he-
lium carbon star.
MW Sgr P var. Max = 2418940 + 202.3d*E (JD2418900 - 23900);
Max = 2428753 + 206.5d*E (JD2423900 - 28950);
since JD2428950 - see Table.
NP Sgr The cycles 100 - 300d
are possible.
OW Sgr In the region of
the open cluster NGC 6716.
V348 Sgr VB A (B 15m pg, 16", 73deg). See MV Sgr.
By the character of
light variation and the spectrum the star is unique.
The light curve resembling those of RCB type stars
is superimposed by conspicuons irregular and semire-
gular variations with the mean cycle about 200d
[2449, 9824]. The star is surrounded by a nebula the
radius of which equals 1". A fainter nebulous envelo-
pe is observed up to 7" from the star. Large infrared
excess. Spectrum description [2451, 9825]. Probably
the star is intermediate between the RCB variables
And planetary nebula Wolf-Rayet central stars.
V350 Sgr SB [9004].
V354 Sgr d = 0.02P.
V356 Sgr Min II 7.24; DII = 0.20P:; d = 0.05P;
0.490P (1928) <= Min II - Min I <= 0.505P (1951).
Apsidal motion is possible.
V366 Sgr P var. Max = 2425479.448 + 0.4779616d*E (JD
2423990 - 28780) [0705]; since JD2435600 -
see Table. [Ca/H] = -0.73.
V367 Sgr [Ca/H] = -1.21.
V377 Sgr The epoch of
light min is given in the Table.
P var. Min = 2426071.24 + 16.17076d*E (JD2425300 -
26600) [0048]; Min = 2427350.25 + 16.19326d*E (JD
2426600 - 28700) [1400]; Min = 2436358.98 + 16.1575d*E
(JD2436200 - 37300); Min = 2437863.09 + 16.1925d*E
(JD2437660 - 39100); Min = 2440114.81 + 16.2407d*E
(JD2440200 - 560); since JD2440950 -
see Table.
V397 Sgr There is a
square term in the elements: -0.009d*10**-6*E**2
V401 Sgr Min II 14.1.
V403 Sgr THere is a
nonlinear term in the elements: -0.013d*10**-6*E**2.
V410 Sgr VB A (B 13.6m, 270deg).
V426 Sgr Min II 13.3.
V427 Sgr There is a
nonlinear term in the elements: -131d*10**-10*E**2.
The shape of the
light curve varies: 0.17P <= M - m <= 0.22P.
V431 Sgr Min II 14.9.
V437 Sgr Min II 14.0.
V440 Sgr delta(S) = 9. P var. P = 0.4774659d (JD2416000 - 23000)
[0752]; P < 0.4774659d (JD2422000 - 26000) [0235];
Max = 2426581.203 + 0.477474d*E (JD2426000 - 29460)
[1000]; since JD2437100 - see
Table.
V453 Sgr There is a
nonlinear term in the elements: +0.003d*10**-6*E**2.
V457 Sgr There is a
nonlinear term in the elements: -0.005d*10**-6*E**2.
V466 Sgr There is a
nonlinear term in the elements: +0.03d*10**-6*E**2.
V496 Sgr Min II 14.3.
V497 Sgr Min II 16.0.
V505 Sgr Min II 6.63. P var. Min I = 2433515.3295 + 1.18287141d*E
(JD2425500 - 35800) [1642]; Min I = 2437494.4964 +
+ 1.1828622d*E (JD2435800 - 37500); Min I =
= 2440055.3991 + 1.1828650d*E (JD2437500 - 40100);
Min I = 2442656.5283 + 1.18286917d*E (JD2440100 -
42670); since JD2442670 - see
Table. The shape of the light curve varies. Deviations
from the mean light curve vary with P = 310d. The
difference of Min I and Min II depths varies by 0.05m
[9830].
V511 Sgr P var. Max = 2423950 + 158.8d*E (JD2411300 - 23950);
since JD2423950 - see Table.
V515 Sgr There is a
nonlinear term in the elements: +0.015d*E**2.
V519 Sgr THere is a
nonlinear term in the elements: +0.0046d*E**2.
V520 Sgr There is a
nonlinear term in the elements: +0.051d*E**2.
V523 Sgr Min II 9.88. Apsidal mo-
tion is observed. In the Table the epoch of Min I is
given corresponding to the moment of line of apsides
coinciding with the line of sight, when Min II - Min I =
= 0.50P. The mean period according to [2453] is given;
with this period O - C deviations do not exceed +-0.06P
for both minima. The period of apsidal motion is 248
years [2453]. Min II - Min I = 0.39P in 1953.
V524 Sgr Min II 11.2.
V525 Sgr Min II 8.51.
V526 Sgr VB A (B 12.40m, 8.6", 7.3deg). Min II 10.20, DII = 0.17P;
dI = 0.006P, dII = 0.013P.
There are periodic terms in the elements:
+ 0.1369d sin (0.01295deg*E) - 0.0115d sin (0.0259deg*E) +
+ 0.0011d sin (0.0388deg*E). Min II = 2422055.0453 +
+ 1.919411d*E - 0.1369d sin (0.01295deg*E) -
- 0.0115d sin (0.0259deg*E) - 0.0011d sin (0.0388deg*E).
The period
of apsidal motion is 146 years. e = 0.224.
V527 Sgr P var. Max = 2426904.95 + 1.258956d*E (JD2425790 -
7650) [1648]; since JD2438200 -
see Table.
V551 Sgr VB B (A 16.5m; B 12", 135deg).
V552 Sgr P var. The elements given in the Table are
valid since JD2418400.
V554 Sgr Min II 14.5.
V557 Sgr P var. Max = 2415110.5 + 16.233d*E (JD2415100 -
22000); Max = 2426100.0 + 16.260d*E (JD2423900 -
27700) [0251]; Max = 2428097.70 + 16.171d*E (JD
2427700 - 28800) [0296]; since JD2428800 -
see Table.
V558 Sgr Min II 14.3.
V564 Sgr P var. Max = 2424056 + 27.8d*E (JD2423780 - 26000)
[0251]; Max = 2428403.3 + 27.99d*E (JD2427870 -
29160) [0296]; Max = 2429158.2 + 27.2d (JD2429150 -
515); since JD2429515 - see
Table.
V567 Sgr The
central star of the planetary nebula P.K.355 -6deg 1
(M3-21).
V573 Sgr Min II 12.7.
V574 Sgr Min II 14.7.
V578 Sgr According to [2448], Max = 2428710 +
+ 253d*E.
V593 Sgr P var. Max = 2414150 + 230d*E (JD2414100 - 22900);
since JD2423900 - see Table.
V598 Sgr d = 0.05P.
V611 Sgr P var. Max = 2414150 + 123d*E (JD2414150 - 19000);
since JD2420250 - see Table.
The period must pro-
bably be doubled because the star resembles RV Tau
(Min II 16.2).
V612 Sgr P var. Max = 2413750 + 107.9d*E (JD2413700 - 17900);
since JD2418800 - see Table.
V615 Sgr P.K.356 -7deg 1 = He 2-349.
V626 Sgr P var? Max = 2427715.4 + 26.745d*E (JD2425380 -
28800) [0046]; since JD2434500 -
see Table.
V631 Sgr Min II 14.2.
V632 Sgr P var. Max = 2413350 + 263d*E (JD2413300 - 19000);
since JD2420200 - see Table.
V633 Sgr P var. Max = 2415110 + 224d:*E (JD2415000 - 18800);
since JD2420000 - see Table.
V638 Sgr P var? Max = 2412670 + 73.1d*E (JD2412600 - 14540);
since JD2414800 - see Table.
V646 Sgr P var. Max = 2413350 + 95d*E (JD2413300 - 15900);
since JD2423900 - see Table.
V660 Sgr P var. Max = 2426460 + 235.6d*E (JD2426400 - 35700)
[0251]; since JD2435600 - see
Table.
V663 Sgr P var. Max = 2426160 + 305d*E [0251]; since
JD2435600 - see Table.
V671 Sgr P = 292.5d?
V672 Sgr P var? Max = 2424680 + 228d*E [0251]; since
JD2435600 - see Table.
V674 Sgr P var. Max = 2425830 + 249d*E [0251]; since
JD2435600 - see Table.
V675 Sgr (k - b)2 = -0.01; delta(S) = 11.
V676 Sgr P var. Max = 2414140 + 181d*E (JD2414100 - 22600)
[0251]; since JD2423900 - see
Table.
V679 Sgr P var. Max = 2415900 + 225d*E (JD2415900 - 22200)
[0251]; Max = 2425440 + 223.1d*E (JD2425000 -
29000); since JD2429000 - see
Table.
V683 Sgr Min II 12.5.
V686 Sgr P var? Max = 2425390 + 225.3d*E [0251]; since
JD2435600 - see Table.
V687 Sgr Min II 12.2.
V691 Sgr P var? Max = 2426095.550 + 0.46911d*E [0251];
since JD2435630 - see Table.
V703 Sgr Var 4. According
to [2951] the range of light variation, the type of va-
riability and the elements of light variation are erro-
neously assigned in [1640] to the star Var.3.
V705 Sgr Min II 12.9.
V710 Sgr P var. Min = 2426101.550 + 2.3817d*E [0251]; Min =
= 2431286.425 + 2.381633d*E (JD2428390 - 35700)
[3513].
V713 Sgr P var? Max = 2424680 + 253.4d*E [0251]; since
JD2435600 - see Table.
V716 Sgr P var? Max = 2424670 + 277d*E [0251]; since
JD2435600 - see Table.
V718 Sgr P var? Max = 2425850 + 153.2d*E [0251]; since
JD2435600 - see Table.
V721 Sgr P = 71:d?
V725 Sgr Unique star.
The mean brightness increased from 13.0m to 12.4m
since 1889 to 1915, and fell to 12.8m in 1926. From
1895 to 1926 real shortperiodic oscillations with the
amplitude about 0.4m. In 1928 the amplitude suddenly
increased by almost 2m, but the magnitude in maxi-
mum remained unchanged. From 1928 to 1935 the light
variations became periodic, the period increasing every
year by 1d in accordance with the formula: Min = 2426087 +
+ 15.933d*E + 0.0233d*E**2. In 1935 P = 21d. Since
1936 only small oscillations of brightness with a
gradual increase of the mean magnitude from 14.3m to
13.9m B (1969). Photoelectric observations in 1968 -
69 reveal the light variations 12.33m - 12.72m V with
possible periods 15.4d in 1968 and 45.3d in 1969. In
1973 12.28m - 12.58m V, = +1.37, P = 50d [7101].
V727 Sgr VB A (B = V728 Sgr, 14.7m - 15.9m, 25", 108deg).
V728 Sgr VB B (A = V727 Sgr, B 25", 108deg).
V734 Sgr Min II 13.1.
V735 Sgr VB A (B 15.5m, 6", 315deg). Accor-
ding to B-V, U-B values and spectrum the star is
not a UG type variable [9840].
V738 Sgr In the region of the
globular cluster NGC 6558.
According to [5403], RV? P = 86.78d?
V743 Sgr Min II 14.2.
V745 Sgr P var. Max = 2416560 + 385.1d*E (JD2411000 - 19260);
since JD2419260 - see Table.
V748 Sgr Min II 14.7; d = 0.04P.
V750 Sgr d = 0.02P:.
V752 Sgr Min II 12.7.
V755 Sgr d = 0.01P.
V757 Sgr Min II 13.8; d = 0.06P.
V760 Sgr Min II 13.4. P var. Min = 2414059.5 + 45.10d*E (JD
2412800 - 19000); since JD2419000 -
see Table.
V761 Sgr Min II 12.8; d = 0.05P.
V762 Sgr P var. Max = 2414100 + 461d*E (JD2411000 - 22860);
since JD2422860 - see Table.
V763 Sgr P var. The observations are satisfied by
the given elements since JD2415000.
V766 Sgr d = 0.05P.
V768 Sgr Min II 13.0.
V770 Sgr Min II 13.1.
V773 Sgr [A/H] = 0.1.
V777 Sgr d = 0.055P.
V778 Sgr Min II 12.1.
V779 Sgr Min II 12.0.
V780 Sgr Min II 12.9; d = 0.08P.
V782 Sgr d = 0.045P.
V784 Sgr Min II 12.8.
V786 Sgr d = 0.025P.
V789 Sgr In the region of
the open cluster Tr 31.
P = 5.10470d (Min II 12.7)? [0478].
V791 Sgr d = 0.03P:.
V792 Sgr Min II 12.2. In the region of the open cluster
And the diffuse nebula NGC 6514 (M 20).
V793 Sgr P var. Max = 2412610 + 195d*E (JD2412600 - 19400);
since JD2423400 - see Table.
V794 Sgr P var. Min I = 2413723 + 173.48d*E (JD2413700 -
23750); since JD2423750 - see
Table.
V801 Sgr Min II 14.9.
V802 Sgr [A/H] = -0.4.
V803 Sgr P = 3.771748d?
V818 Sgr The shape of the
light curve varies.
V819 Sgr P var?
V824 Sgr Min II 15.2.
V828 Sgr There is a close companion.
V838 Sgr P var?
V839 Sgr P var? Max = 2426170.126 + 1.835347d*E (JD2425700 -
26600) [1598]; since JD2441500 -
see Table.
V841 Sgr see V818 Sgr.
V844 Sgr P var?
V845 Sgr Min II 14.6.
V859 Sgr see V818 Sgr.
V879 Sgr see V828 Sgr.
V882 Sgr Min II 14.6.
V884 Sgr 0.20P <= M - m <= 0.40P. Blazhko effect.
V889 Sgr 0.14P <= M - m <= 0.24P. Blazhko effect.
V902 Sgr Min II 14.8.
V903 Sgr Min II 13.0.
V919 Sgr Spectrum description [9845].
V935 Sgr P var. Max = 2420040 + 232.0d*E (JD2419500 - 28650);
since JD2428600 - see Table.
V938 Sgr P = 138.27d?
V960 Sgr nP = 1734d.
V966 Sgr Min II 14.0.
V977 Sgr d = 0.03P.
V981 Sgr Min II 14.8.
V985 Sgr Min II 14.3.
V986 Sgr d = 0.015P.
V993 Sgr dI = 0.05P:; Min II 13.7, DII = 0.09P, dII = 0.00P.
V994 Sgr Min II 12.8:.
V998 Sgr The depth of Min II 0.04m:.
V1000 Sgr Min II 13.9.
V1002 Sgr Min II 13.7.
V1004 Sgr [A/H] = -0.2.
V1005 Sgr Min II 13.9.
V1013 Sgr Min II 15.0.
V1017 Sgr VB B (A 10.6m V; B 15", 270deg).
For a long time the star was
considered to be a recurrent nova. Three considerable
flares were observed: in 1901 (10.8m), 1919 (6.2m),
And 1973 (10.5m). Composite spectrum with a trace
of a hot component [3872].
V1023 Sgr In the region of
the open cluster Cr 394. Min II 13.0:.
V1026 Sgr Min II 13.4.
V1028 Sgr Min II 14.4.
V1032 Sgr Min II 15.0.
V1033 Sgr See V818 Sgr. Blazhko
effect?
V1034 Sgr d = 0.025P:.
V1049 Sgr Min II 13.6; Min II - Min I = 0.326P; DII = 0.025P.
V1050 Sgr Min II 14.1.
V1056 Sgr Min II 14.1.
V1063 Sgr The shape of the light curve strongly vari-
es. Blazhko effect?
V1068 Sgr Min II 15.4.
V1069 Sgr See V1063 Sgr.
V1071 Sgr P = 1.3560996d?
V1072 Sgr See V1063 Sgr.
V1080 Sgr P var. See V818 Sgr.
V1081 Sgr P var?
V1089 Sgr Cycle <= 30d.
V1100 Sgr d = 0.02P:.
V1108 Sgr Min II 11.9; Min II - Min I = 0.516P.
V1109 Sgr Min II 14.5.
V1127 Sgr THere is a
nonlinear term in the elements: +78.10d**-10*E**2.
V1136 Sgr d = 0.020P.
V1148 Sgr In the region of the
globular cluster NGC 6553.
V1153 Sgr P var? Max = 2428391.266 + 1.332624d*E (JD2427680 -
30910); since JD2435630 - see
Table.
V1177 Sgr Min II 11.4.
V1178 Sgr d = 0.03P:.
V1180 Sgr [A/H] = -0.4.
V1181 Sgr [A/H] = 0.6. P var. Max = 2428452.25 + 21.341d*E (JD
2427400 - 31000) [1638]; since JD2433000 -
see Table.
V1185 Sgr [A/H] = -0.5. P var. Max = 2428778.86 + 13.9123d*E
(JD2427500 - 32750) [1638]; Max = 2437485.4 +
+ 13.901345d*E (JD2437100 - 43760) [8519];
since JD2444000 - see Table.
V1187 Sgr [A/H] = -0.8.
V1188 Sgr [CA/H] = -0.37.
V1189 Sgr [A/H] = -1.1.
V1190 Sgr P = 3.000078d?
V1191 Sgr Min II 14.4.
V1205 Sgr The alternative
period is possible: 0.659820d [1638].
V1209 Sgr A var.
V1211 Sgr delta(S) = 3:.
V1214 Sgr There is a
nonlinear term in the elements: -0.25d*10**-7*E**2.
V1216 Sgr mu = 0.720", P = 106.7deg.
V1223 Sgr As a rule
has a persistent high state; five drops by two to more
than three magnitudes have been registered And a
twelve year interval of irregular variations at inter-
mediate magnitudes.
According
To [9850] there are slow variations in brightness by
0.15m on a time scale of ~ 1 day. They are superimpo-
sed by variations with the orbital period P orb (Max =
= 2444749.9866 + 0.140239d*E) and with amplitude up
to 0.15m. These variations in their turn are superimpo-
sed by the others: with P = 794.38s and the amplitude
from 0.03m up to 0.15m (Max = 2444750.00404 +
+ 0.009194215d*E and (sometimes) with P = 849.8s and
a twice smaller amplitude (Max = 2444750.00350 +
+ 0.00983588d*E). Besides there are rapid brightness
variations on time scales 10 - 100s by 0.10m - 0.20m,
and high frequency flickering by 0.05m. According to
[9851], the period of X-ray pulses associated with
the rotation of the compact object is 12.5 minutes.
V1276 Sgr Min II 14.3.
V1280 Sgr Brightness of Max varies by 2m with the period
5230d.
V1281 Sgr The light
variation is not strictly periodic.
V1282 Sgr P var. Min = 2427651.297 + 1.754574d*E (JD2427650 -
30560) [0705]; since JD2435600 -
see Table.
V1284 Sgr Min II 13.5. EB?
V1287 Sgr See V703 Sgr.
Var 3.
According to [2951] the range of light variation, the type
of variability and the elements of light variation are
erroneously assigned in [1640] to the star Var 4.
Min II 14.8.
V1290 Sgr [A/H] = -1.2.
V1303 Sgr [A/H] = -0.8. P var? Max = 2438241.176 + 18.46812d*E
(JD2427700 - 38250) [0001]; since JD
2444000 - see Table.
V1304 Sgr [A/H] = 0.3. P var. Max = 2428758.10 + 12.9287d*E
(JD2427590 - 28820) [1640]; since JD
2435600 - see Table.
V1309 Sgr Not far from V4032 Sgr.
V1311 Sgr V 14 in the globular clus-
ter NGC 6656 (M22).
Not a member of the cluster.
V1312 Sgr P var? Max = 2428815.600 + 0.6011427d*E (JD
2427590 - 28820) [1640]; since JD2435630 -
see Table.
V1314 Sgr P var? Max = 2428346.536 + 0.657489d*E (JD2427600 -
28820) [1640]; since JD2435630 -
see Table.
V1317 Sgr P var?
V1327 Sgr SR?, L? [8424].
V1328 Sgr P = 0.39937d?
V1329 Sgr VB B (A 17.2m; B 1.4", 120deg). P var. Max = 2432388.777 +
+ 0.48306d*E (JD2431670 - 32740) [3524];
since JD2443300 - see Table.
V1331 Sgr Min II 16.5.
V1352 Sgr P var. Max = 2431998.851 + 0.49505d*E (JD2431670 -
33150) [1680]; Max = 2443341.844 + 0.49493d*E (JD
2443300 - 350); Max = 2444087.558 + 0.49516d*E (JD
2444050 - 110); in the interval JD
2444400 - 410 - see Table.
V1356 Sgr Min II 18.0:.
V1357 Sgr Min II 19.0.
V1359 Sgr P var?
V1369 Sgr P var. Max = 2432736.821 + 0.52956d*E (JD2431670 -
33150) [3524]; since JD2440700 -
see Table.
V1374 Sgr delta(S) = 1.
V1378 Sgr delta(S) = -3:.
V1387 Sgr delta(S) = 3.
V1389 Sgr The epoch of Min brightness
is given.
V1390 Sgr Min II 17.6.
V1392 Sgr P var. Max = 2432739.791 + 0.55032d*E (JD2431670 -
33150) [3524]; since JD2440700 -
see Table.
V1393 Sgr delta(S) = 3.
V1394 Sgr Min II 18.0.
V1401 Sgr See V1389 Sgr.
V1405 Sgr P var. Max = 2432031.778 + 0.46511d*E (JD2431670 -
33150) [6094]; since JD2443300 -
see Table.
V1408 Sgr A var (0.5m <= A <= 1.4m).
V1409 Sgr P var. Max = 2432739.822 + 0.65159d*E (JD2431670 -
33150) [3524]; since JD2443300 -
see Table.
V1412 Sgr See V1389 Sgr.
V1415 Sgr P var?
V1416 Sgr delta(S) = 3. P var? Max = 2432002.875 + 0.42767d*E
(JD2431670 - 33150) [6094]; since JD
2440700 - see Table.
V1418 Sgr P var. Max = 2432740.818 + 0.45423d*E (JD2431670 -
33150) [3524]; since JD2440700 -
see Table.
V1419 Sgr P var. Max = 2432061.669 + 0.57144d*E (JD2431670 -
33150) [1680]; since JD2440700 -
see Table.
V1425 Sgr Min II 18.8.
V1426 Sgr delta(S) = 1.5.
V1429 Sgr See V1389 Sgr.
V1435 Sgr Min II 18.0; Min II - Min I = 0.53P.
V1437 Sgr V8 (NGC 6522); not a
member of the globular cluster.
V1438 Sgr V9 (NGC 6522); not a
member of the globular cluster.
V1439 Sgr P = 0.53711d? [6094].
V1443 Sgr Min II 18.6.
V1446 Sgr Min II 18.0.
V1447 Sgr Min II 18.2.
V1454 Sgr Min II 15.4.
V1457 Sgr Min II 19.0.
V1459 Sgr The depth of Min II is 0.04m.
V1460 Sgr P var. Max = 2432067 + 162.0d*E (JD2431670 - 33150)
[1680]; since JD2440340 - see
Table.
V1464 Sgr delta(S) = 1.
V1465 Sgr P var. Max = 2431702.660 + 0.45757d*E (JD2431700 -
940); Max = 2432706.945 + 0.45757d*E (JD2431940 -
32740) [3524]; since JD2440740 -
see Table.
V1466 Sgr see V1389 Sgr.
V1473 Sgr According to [8424] P = 340d.
V1487 Sgr Min II 18.8.
V1491 Sgr Min II 18.5.
V1498 Sgr SP component of a close
pair. P var. Max = 2432739.728 + 0.47467d*E
(JD2431670 - 33150) [6094]; since JD
2443300 - see Table.
V1508 Sgr VB.
V1509 Sgr Min II 18.1:.
V1510 Sgr According to [6094], P = 0.48546d.
V1516 Sgr P var? Max = 2432740.753 + 0.49709d*E (JD2431670 -
33150) [3524]; since JD2440700 -
see Table.
V1517 Sgr P < 2.0d.
V1523 Sgr P var? Max = 2432417.702 + 0.36202d*E (JD2431670 -
33150) [3524]; since JD2443300 -
see Table.
V1526 Sgr Min II 18.3.
V1537 Sgr Min II 17.4; Min II - Min I = 0.54P.
V1540 Sgr According to [8424], P = 465d.
V1546 Sgr See V1389 Sgr.
V1550 Sgr P = 0.37432d? [6094].
V1554 Sgr Min II 17.5.
V1557 Sgr delta(S) = 8.
V1558 Sgr delta(S) = 1.
V1559 Sgr See V1459 Sgr.
V1561 Sgr Min II 17.7.
V1567 Sgr Min II 18.0.
V1569 Sgr Min II 18.6.
V1576 Sgr [Ca/H] = -1.23.
V1577 Sgr P var. Max = 2426200 + 290d*E (JD2426000 - 30560)
[2449]; since JD2430560 - see
Table.
V1580 Sgr P var (310d <= P <= 365d).
V1589 Sgr [Ca/H] = -0.91.
V1602 Sgr d = 0.03P.
V1610 Sgr P < 0.5d.
V1639 Sgr See V818 Sgr.
V1640 Sgr (k -b)2 = 0.24. P var?
V1642 Sgr 250d <= P <= 350d.
V1643 Sgr Min II 12.1. According to [5771], RR?, P =
= 0.34d.
V1644 Sgr See V818 Sgr.
V1647 Sgr VB A (B 9.13m, 8", 104deg). Min II 7.43, DII = 0.059P,
Min II - Min I = 0.262P (JD2441830); Min II =
= 2441830.55561 + 3.28282227d*E.
The apsidal motion period is 592.5 +- 6.5 years.
V1648 Sgr Close VB. Flat Min.
V1652 Sgr See V1648 Sgr.
V1653 Sgr See V1648 Sgr.
V1656 Sgr See V1648 Sgr.
V1658 Sgr P var.Max = 2426560 + 105d*E (JD2417000 - 28000)
[0842]; since JD2428000 - see
Table.
V1660 Sgr See V1648 Sgr.
V1661 Sgr See V1648 Sgr.
P var. Max = 2426850 + 275d*E (JD2424000 - 26850);
since JD2436700 - see Table.
V1667 Sgr P var. Max = 2426560 + 158d*E (JD2417000 - 36000)
[0842]; since JD2436000 - see
Table.
V1668 Sgr See V1648 Sgr.
V1670 Sgr A var. P var. The shape of the
light curve varies (probably with a period of about
11 years).
V1675 Sgr A possible companion of
16m.
V1679 Sgr See V1648 Sgr.
V1681 Sgr See V1675 Sgr.
V1690 Sgr See V1675 Sgr.
V1691 Sgr See V1648 Sgr.
P var. Max = 2426520 + 235d*E (JD2417000 - 28000)
[0842]; since JD2436000 - see
Table.
V1697 Sgr See V1675 Sgr.
V1698 Sgr See V1675 Sgr.
V1699 Sgr P var. Max = 2425410 + 203.6d*E (JD2417000 - 27600)
[0842]; since JD2436000 - see
Table.
V1703 Sgr See V1675 Sgr.
V1705 Sgr P var. Max = 2425860 + 142d*E (JD2417000 - 27000)
[0842]; since JD2435800 - see
Table.
V1711 Sgr [A/H] = -1.1. P var. Max = 2435365.19 + 30.46d*E
(JD2432700 - 35400) [2570]; since JD
2442200 - see Table.
V1714 Sgr In the region of
the open cluster ruprecht 134.
V1721 Sgr d = 0.03P:.
V1723 Sgr Min II 13.8.
V1730 Sgr Min II 14.8:; d = 0.03P:.
V1741 Sgr In the nebula and the
cluster NGC 6530 (M8). Var1.
V1743 Sgr See V1741 Sgr. Var 2.
V1747 Sgr See V1741 Sgr. Var 3.
V1748 Sgr See V1741 Sgr. Var 4.
V1749 Sgr See V1741 Sgr. Var 6.
V1750 Sgr See V1741 Sgr. Var 8.
V1751 Sgr See V1741 Sgr. Var 7.
V1752 Sgr See V1741 Sgr. Var 13.
V1753 Sgr See V1741 Sgr. Var 14.
V1755 Sgr See V1741 Sgr. Var 15.
V1758 Sgr See V1741 Sgr. Var 16.
V1761 Sgr See V1741 Sgr. Var 19.
V1762 Sgr See V1741 Sgr. Var 20.
V1764 Sgr See V1741 Sgr. Var 23.
V1765 Sgr See V1741 Sgr. Var 24.
V1768 Sgr See V1741 Sgr. Var 26.
V1769 Sgr See V1741 Sgr. Var 27.
V1771 Sgr See V1741 Sgr. Var 29.
V1772 Sgr See V1741 Sgr. Var 28.
V1773 Sgr See V1741 Sgr. Var 31.
V1774 Sgr See V1741 Sgr. Var 30.
V1775 Sgr See V1741 Sgr. Var 33.
V1776 Sgr See V1741 Sgr. Var 36.
V1777 Sgr See V1741 Sgr. Var 37.
V1778 Sgr See V1741 Sgr. Var 34.
V1779 Sgr See V1741 Sgr. Var 40.
V1780 Sgr See V1741 Sgr. Var 39.
V1781 Sgr See V1741 Sgr. Var 41.
V1782 Sgr See V1741 Sgr. Var 44.
V1784 Sgr See V1741 Sgr. Var 45.
V1785 Sgr See V1741 Sgr. Var 46.
V1786 Sgr See V1741 Sgr. Var 48.
V1787 Sgr See V1741 Sgr. Var 47.
V1788 Sgr See V1741 Sgr. Var 50.
V1789 Sgr See V1741 Sgr. Var 51.
V1790 Sgr See V1741 Sgr. Var 49.
Western component of a close pair.
V1791 Sgr See V1741 Sgr. Var 53.
V1792 Sgr See V1741 Sgr. Var 55.
V1793 Sgr See V1741 Sgr. Var 54.
V1794 Sgr See V1741 Sgr. Var 56.
V1795 Sgr See V1741 Sgr. Var 58.
V1797 Sgr See V1741 Sgr. Var 59.
V1798 Sgr See V1741 Sgr. Var 60.
V1800 Sgr See V1741 Sgr. Var 61.
V1801 Sgr See V1741 Sgr. Var 62.
V1802 Sgr See V1741 Sgr. Var 63.
V1803 Sgr See V1741 Sgr. Var 64.
SP component of a close pair.
V1805 Sgr See V1741 Sgr. Var 66.
V1807 Sgr See V1741 Sgr. Var 67.
V1808 Sgr See V1741 Sgr. Var 68.
V1828 Sgr P var. Max = 2424402 + 12.985d*E (JD2423800 -
36000) [2515]; since JD2436000 -
see Table.
V1831 Sgr P var. Max = 2428849.4 + 26.58d*E (JD2427500 -
31270) [2447]; since JD2435630 -
See Table.
V1843 Sgr P = 163.7d? [5869].
V1845 Sgr Flat Min. Close
companion?
V1864 Sgr Epoch of light maxi-
mum is given.
V1869 Sgr P var. Max = 2434178 + 346d*E (JD2427590 - 34220)
[2447]; since JD2435630 - see
Table.
V1882 Sgr See V818 Sgr.
V1891 Sgr A companion of 16m.
V1894 Sgr V4 (NGC 6637).
Possible member of the globular cluster NGC
6637 (M 69).
V1895 Sgr P var. Max = 2421065 + 156.0d*E (JD2418850 - 21100);
since JD2427600 - see Table.
V1900 Sgr A companion of 15m.
V1904 Sgr See V1900 Sgr.
V1911 Sgr P var. Max = 2428832.4 + 10.0581d*E (JD2427600 -
34220) [2447]; since JD2435630 -
See Table.
The shape of the
light curve varies?
V1925 Sgr P var?
V1942 Sgr In the region of
the open cluster Ruprecht 147.
V1945 Sgr See AU Sgr.
V1946 Sgr See AU Sgr.
V1947 Sgr See AU Sgr. All the published charts
for this variable are wrong. According to [9861] the
star actually lies 1.1 mm south and 0.8 mm east of
"D2" in fugure 3 published in [2428].
V1948 - V1951 Sgr
See AU Sgr.
V1954 Sgr VB(ro = 2"). P var.
There is a nonlinear term in the elements:
-4.1313d*10**-8*E**2.
V1958 Sgr Min II 14.0.
V1962 Sgr In the region of the open cluster And the
diffuse nebula NGC 6618 (M 17).
V1963 Sgr See V1962 Sgr.
V1966 Sgr See V1962 Sgr.
V1969 Sgr There
are three close faint companions (15.8m-16.3m).
V1970 Sgr See V1962 Sgr.
V1971 Sgr See V1962 Sgr.
V1973 Sgr See V1962 Sgr.
V1975 Sgr See V1962 Sgr.
The presence of a blue companion is pos-
sible.
V1976 - V1977 Sgr
See V1962 Sgr.
V1980 Sgr Min II 11.7; DII = 0.11P; Min II - Min I = 0.52P.
V1996 Sgr VB.
V2003 Sgr S 5.5/5. See Y Sgr.
V2007 Sgr V 26 (NGC 6656 = M 22).
V2008 Sgr P = 120 - 135d.
V2028 Sgr In the region of the
globular cluster ngc 6681 (M 70).
V2037 Sgr A close companion is
possible.
V2054 Sgr P > 450d?
V2064 Sgr VB.
Combined brightness of the star and the close compa-
nion was estimated. It is not clear which star is vari-
able.
V2065 Sgr NP component of a clo-
se binary.
V2094 Sgr P < 0.5d.
V2106 Sgr VB.
Combined brightness of the components was estima-
ted.
V2148 Sgr See V2106 Sgr.
The variable
is the nortHern component.
V2276 Sgr P < 30d.
V2282 Sgr Star L. See V1945 Sgr.
Late spectrum.
V2283 Sgr Min II 10.59:.
Apsidal motion with P = 560 years [7107]:
0.739P (1898) <= Min II - Min I <= 0.797P (1965).
THere are periodic terms in the
elements given in the Table:
+ 0.5414d sin 0.006deg (E + 45019) - 0.0995d sin 0.012deg*
(E + 45019) + 0.0217d sin 0.018deg (E + 45019); Min II =
= 2438946.7619 + 3.4714231d*E - 0.5414d sin 0.006deg*
(E + 45019) - 0.0995d sin 0.012deg (E + 45019) - 0.0217d*
sin 0.018deg (E + 45019).
V2284 Sgr P var.
V2285 Sgr In the region of the
globular cluster NGC 6558.
V2313 Sgr Min II 16.8.
V2315 Sgr P = 0.193d?
V2323 Sgr Blue [8424].
V2341 Sgr See V1389 Sgr.
V2342 Sgr V 17 (NGC 6626 = M28).
The member of this globular cluster. Min II 13.5.
V2343 Sgr A close companion of 14.5m.
V2346 Sgr Cycles 50 - 100d.
V2349 Sgr Min II 9.2.
V2351 Sgr Min II 10.31.
V2352 Sgr P var.
There is a nonlinear term in the elements:
+ 0.0525d*E**2.
V2355 Sgr In the region of the
globular cluster NGC 6637 (M 69).
V2358 Sgr In the region of the
globular cluster NGC 6642.
V2359 - V2361 Sgr
See V2355 Sgr.
V2362 Sgr A close companion of 15m.
V2366 Sgr P var.
There is a nonlinear term in the elements:
+ 0.6815d*10**-9*E**2.
V2367 Sgr V28 (NGC 6656 = M22).
Not a member of this globular cluster.
P = 323d?
V2378 Sgr Two close
companions of 15.3m and 15.8m.
V2389 Sgr P var?
V2391 Sgr P = 189d?
V2413 Sgr P Var. The ele-
ments are valid in the interval JD2425440 - 30905.
V2416 Sgr P.K. 7 +1G 2.
V2425 Sgr E?
V2442 Sgr P = 0.5d?
V2449 Sgr Min II 17.4.
V2468 Sgr See V2323 Sgr.
V2471 Sgr VB B (A 14.6m; B 8", 225deg).
V2493 Sgr See V2323 Sgr.
V2506 Sgr P.K. 3 -4deg 6.
V2507 Sgr Min II 14.6.
V2508 Sgr Min II 14.1:.
V2509 Sgr Min II 7.50.
V2510 Sgr See V1389 Sgr.
The ele-
ments given in the Table are valid since JD
2427440.
V2520 Sgr VB.
V2526 Sgr See V1389 Sgr.
P var. Min = 2428699.5 + 31.3224d*E (JD2424100 -
31400) [5590]. Since JD2431400 -
See Table.
V2529 Sgr Min II 14.5.
Twice shorter period is given in [5590].
V2540 Sgr P var.
V2544 Sgr VB?
V2552 Sgr VB A (B 15.7m).
V2553 Sgr THere are two close compa-
nions.
V2562 Sgr NortHern component of a close pair. The companion
is of 16m.
V2563 Sgr P var.
V2564 Sgr P var?
V2565 Sgr VB B (A 12.5m; B 90deg).
V2566 Sgr P var. [Ca/H] = -0.52.
V2567 Sgr [Ca/H] = -0.57.
V2568 Sgr P var?
V2576 Sgr P var. Max = 2426200 + 149d*E (JD2423500 - 27000);
since JD2433000 - see Table.
V2577 Sgr P var?
V2578 Sgr VB. See V2358 Sgr.
V2579 Sgr P var. Max = 2429926.251 + 0.5911903d*E (JD2427590 -
34200) [5590]; since JD2435600 -
See Table.
V2584 Sgr P var. Max = 2426564.347 + 0.534829d*E (JD2423940 -
33860); since JD2437820 - see
Table.
V2592 Sgr In the region of the
gLobular cluster NGC 6656 (M22).
V2593 Sgr P var. Max = 2428780.349 + 0.5123825d*E (JD
2427680 - 34200) [5590]; since JD2435600 -
see Table.
V2594 Sgr P var.
V2598 Sgr A companion 15.8m.
Spectrum description [6495].
V2601 Sgr P.K. 12 -7deg 1. See V1389 Sgr.
V2610 Sgr P var.
V2616 Sgr Min II 13.0.
V2617 Sgr Min II 9.63.
V2620 Sgr P = 185.6d?
V2625 Sgr P = 0.75837d?
V2628 Sgr P = 171d:?/205d:?/256d:?.
V2645 Sgr P var?
V2649 Sgr P = 143d:?
V2672 Sgr P = 196.8d? /204.5d, /255.3d? /315.0d?
V2682 Sgr P = 228.5d?
V2687 Sgr P = 174d:?
V2703 Sgr P = 270d:?
V2719 Sgr SR?
V2731 Sgr P = 147d:?
V2732 Sgr P = 188.6d?
V2733 Sgr P = 244d:?
V2736 Sgr [Ca/H] = -1.45.
V2738 Sgr [Ca/H] = -0.67.
V2740 Sgr P = 269.0d?
V2745 Sgr [Ca/H] = -1.15.
V2756 Sgr P.K. 2 -5deg 1. See V1389 Sgr.
V2763 Sgr P = 216d:?
V2777 Sgr [Ca/H] = -0.83.
V2783 Sgr P = 265.0d?
V2789 Sgr P = 255.5d?
V2798 Sgr P = 244.5d?
V2816 Sgr P = 250d:?
V2828 Sgr P = 0.39669d?
V2830 Sgr Cepheid?
V2833 Sgr P = 224.0d?
V2834 Sgr P = 275d:?
V2846 Sgr P = 0.39659d?
V2868 Sgr P = 235.5d?
V2876 Sgr Min II 15.7:.
V2877 Sgr P = 254.5d?
V2893 Sgr P = 250d:?
V2900 Sgr P = 0.49835d?
V2905 Sgr Spectrum description [4452,
6495].
V2918 Sgr P = 197d:?
V2937 Sgr [Ca/H] = -0.75.
V2947 Sgr RV Tau? Cepheid?
V2959 Sgr P = 0.37233d?
V2962 Sgr P = 209.5d?
V2967 Sgr P = 0.68750d?
V2988 Sgr P = 213.0d? See V3033 Sgr.
V2996 Sgr See V2947 Sgr.
V3004 Sgr [Ca/H] = -0.76.
V3005 Sgr See V2947 Sgr.
V3016 Sgr P var?
V3032 Sgr P = 153d:?
V3033 Sgr The coor-
dinates given in [5869] are erroneous.
V3034 Sgr P = 154d:?
V3038 Sgr P = 252d:?
V3052 Sgr See V2947 Sgr.
V3062 Sgr EW? P = 0.59610d?
V3065 Sgr P = 179.8d?/215.5d?
V3071 Sgr P = 291d:?
V3072 Sgr P = 194d:?
V3088 Sgr P = 215d:?
V3105 Sgr [Ca/H] = -0.82.
V3106 Sgr P = 261d:?
V3111 Sgr P = 182.8d?
V3127 Sgr UG? Not red.
V3128 Sgr Nova? Only one Max
was observed.
V3170 Sgr [Ca/H] = -0.82.
V3175 Sgr P = 179.8d?
V3176 Sgr P = 197d:?
V3179 Sgr P = 297d:?
V3186 Sgr [Ca/H] = -1.28.
V3190 Sgr P = 227.0d?
V3196 Sgr See V2947 Sgr.
V3207 Sgr P = 237d:?
V3239 Sgr P = 226d:?
V3249 Sgr UG?
V3285 Sgr P = 173.8d /196.2d?
V3294 Sgr P = 121d:? /177d:?
V3295 Sgr P = 197d:?
V3335 Sgr See V2947 Sgr.
V3353 Sgr P var?
V3356 Sgr P = 239.5d?
V3365 Sgr P = 197d:? /252d:?
V3388 Sgr P = 125d:? /160d:?
V3395 Sgr P = 159d:?
V3412 Sgr See V2830 Sgr.
V3433 Sgr P = 287.0d?
V3443 Sgr P = 177.6d?
V3444 Sgr P = 160d:?
V3459 Sgr P var. See V818 Sgr.
V3467 Sgr See V2947 Sgr.
V3473 Sgr SR?
V3500 Sgr See V2947 Sgr.
V3501 Sgr Min II 15.7:.
V3508 Sgr The member of the
open cluster M25 (IC 4725).
V3511 Sgr See V2947 Sgr.
V3536 Sgr P = 239.5d?
V3537 Sgr P = 318.0d?
V3551 Sgr P = 165.2d? /201.0d?
V3560 Sgr P = 181d:?
V3564 Sgr See V2830 Sgr.
V3566 Sgr P = 249.0d?
V3583 Sgr P = 228.0d?
V3588 Sgr [Ca/H] = -0.69.
V3625 Sgr P = 294d:?
V3634 Sgr P = 145d:?
V3645 Sgr See Y Sgr.
V3709 Sgr P = 240.0d?
V3718 Sgr P var. There is a nonlinear term
in the elements: +0.865d*10**-10*E**2.
V3748 Sgr P = 0.305327d?
V3765 Sgr [Ca/H] = -0.78.
V3783 Sgr See V2028 Sgr.
V3784 Sgr P = 176.4d?
V3788 Sgr See CC Sgr.
Red.
V3791 Sgr See AU Sgr.
V3792 Sgr VB A (B 8.92m, 13.3", 90deg). Min II 6.81.
The range of
the combined light variation is given in the Table.
See V818 Sgr.
V3804 Sgr Spectrum description [6495, 7099].
V3811 Sgr P2 = 4d? Spectrum description
[7099, 9845].
V3817 Sgr VB A (B 16m).
V3819 Sgr P var.
There is a nonlinear term in the elements:
+10**-10*E**2.
V3829 Sgr A close companion.
V3832 Sgr See V3829 Sgr.
V3834 Sgr Cepheid or eclipsing?
V3837 Sgr P = 0.565d? [6383].
V3838 Sgr VB A (B 15.8m).
V3841 Sgr P var. Max = 2431970 + 358d*E (JD2423900 - 33000);
Since JD2433000 - see Table.
V3842 Sgr A close companion with M2? spectral
class possibly exists.
V3843 Sgr See V2358 Sgr.
V3853 Sgr V22 (NGC 6656 = M22).
The member of this globular cluster.
V3855 Sgr V31 (NGC 6655 = M22).
Possible member of the cluster.
V3857 Sgr According to [6278]
the spectral class is M8.
V3867 Sgr Under the chart S 4903 is printed erroneo-
usly instead of CSV 4309.
V3868 Sgr P var. Max = 2426130 + 270d*E (JD2423900 - 33900);
since JD2435700 - see Table.
V3874 Sgr P var. Max = 2436035 + 115.3d*E (JD2426000 - 38000);
since JD2438000 - see Table.
V3875 Sgr P var. P = 358d (JD2424000 - 33800); since
JD2435000 - see Table.
V3876 Sgr P var. Max = 2430090 + 345d*E (JD2423900 - 32000);
Max = 2436830 + 358d*E (JD2436000 - 41500) [6279];
since JD2441400 - see Table.
V3879 Sgr VB (delta(m) = 2.6m, ro = 0.6").
V3880 Sgr OH, SiO, H2O maser.
V3885 Sgr Porb = 0.206d [4939].
Besides the irregular variability high-fre-
quency oscillations are sometimes observed with
P1 = 29.0s, P2 = 30.15s and with amplitudes of 0.00028m.
In the spectrum tHere are extremely broad absorption
lines of HI and HeI. The Balmer lines have emission
components. X-ray source.
V3886 Sgr Type EB?
V3893 Sgr Connected with
a ring nebula.
V3894 Sgr Min II 6.37. P var?
V3899 Sgr See AU Sgr.
V3900 Sgr V7 (NGC 6522).
Not a member of this globular cluster.
V3903 Sgr The member of the
open cluster Collinder 367.
In the nebula Simeis 188.
V3907 Sgr See V1389 Sgr.
V3929 Sgr P.K.5 -5deg 2.
V3961 Sgr SB1 (Porb = 690d [9915]).
V4024 Sgr SB.
V4032 Sgr Not far from V1309 Sgr.
V4034 Sgr See V1845 Sgr.
V4046 Sgr Flares (11.1m - 12.4m U).
V4048 Sgr Min II 12.6; DII = 0.15P.
V4051- V4056 Sgr
In the region
of the globular cluster NGC 6638.
Not a member of the
cluster.
V4058 Sgr d = 0.02P
V4060 Sgr P var. Max = 2437846 + 283d*E (JD2436030 - 38970);
since JD2438970 - see Table.
V4066 Sgr d ~ 0.07P.
V4067 Sgr V32 (NGC 6656 = M22).
Not a member of the globular cluster.
V4068 Sgr V17 (NGC 6656 = M22).
Not a member of the globular cluster.
V4069 Sgr V33 (NGC 6656 = M22).
Not a member of the globular cluster.
eta Sgr VB A (B 8.0m, 3.5",105deg); mu alfa = -0.0107s, mu .
delta = -0.166"
mu Sgr VB A (B 10.48m, 16.9", 285deg; C 13.0m, 25.2", 119deg;
D 9.69m, 48.5", 312deg; E 9.25m, 50.0", 115deg). SB 2
(e = 0.4).
The variability type is EA/GS +
+ ACYG.
According to [9922]
there are also quasiperiodical light variations with
the amplitudes 0.08m - 0.15m and cycles from 16d to
40d.
ips Sgr Min II 4.59.
R Sco V7 (NGC 6093 = M80). Pro-
bable field star.
P var. Max = 2400518 + 220.2d*E (JD2400500 - 04000)
[0960]; Max = 2404493 + 225.86d*E (JD2404000 -
08600); Max = 2409003 + 222.29d*E (JD2408600 -
33300); since JD2433300 - see
Table.
S Sco V6 (NGC 6093 = M80). Cluster
non-member.
P var. Max = 2400986 + 177.00d*E (JD2400900 - 17500);
since JD2417500 - see Table.
T Sco 4.0" N, 2.7" E from the center of the
globular cluster NGC 6093 = M80.
U Sco Previous outbursts:
2401646: (1863), 2417343 (1906), 2428342 (1936).
Y Sco Since 1972
varies its brightness in the range 12.3m-15.0m irregu-
larly, maxima are unpredictable [8080].
Z Sco P var. Max = 2425546 + 357.17d*E (JD2412500 -
25600); since JD2430000 - see
Table.
RR Sco SiO maser.
P var. Max = 2416944 + 284.31d*E (JD2411000 -
18000); Max = 2422828 + 278.09d*E (JD2422800 -
40000); since JD2440000 - see
Table.
RU Sco P var. During JD2425000 - 40000 -
see Table.
RV Sco VB A (B 13.0m, 5.9", 325deg).
RW Sco OH, H2O, SiO maser.
RY Sco P var, nonlinear term:
+ 4.10d*10**-6*E**2. [A/H] = 0.2.
VB A (B 10.70m, F8:, 13.8", 220.5deg, 1965;
C 11.5m, 2.0", 102deg, 1964; D 11.43m, 24", 80deg).
Combined brightness of AC is
given.
RZ Sco P var. Max = 2413994 + 161.20d*E (JD2413600 -
22700); Max = 2422858 + 155.79d*E (JD2422700 -
28000); Max = 2428156 + 160.29d*E (JD2428000 -
35000); since JD2437500 - see
Table.
SV Sco P var. Max = 2418886 + 258.5d:*E (JD2411600 -
19000); Max = 2424233 + 252.43d*E (JD2420500 -
28600); Max = 2429055 + 255.9d:*E (JD2428600 -
35000); since JD2437000 - see
Table.
SY Sco In the region of
the open cluster NGC 6475 = M7.
TX Sco See SY Sco. Pro-
bable cluster member.
XX Sco The elements Max = 2413786 + 152d*E
[0031] do
not represent the observations from [9447].
AC Sco According to [0266], CST:, 12.2m - 12.6m pg.
AH Sco OH, H2O, SiO maser.
AI Sco P2 = 966.6d.
AL Sco Min II 11.3.
AN Sco EA type is possible.
AP Sco According to [9447], 13.5m - 14.2m pg;
Doubtful identification.
AR Sco According to
[7104], T Tau type spectrum.
AU Sco VB A (B = V725 Sco, 0.4', 0deg).
AV Sco The chart and data in [9447] correspond to
another star.
BI Sco VB B (A = GW Sco; B 6", 150deg).
BM Sco In the region of
the open cluster NGC 6405 = M6.
BN Sco See SY Sco.
Resembles R Cen.
BS Sco d <= 0.03P. According to [0021], SP F8.
BT Sco P var.
There is periodic term in
the elements given in the Table: +0.05d sin (176deg +
+ 0.0857deg*E).
Blazhko effect?
BV Sco Doubtful
identification in [9447].
CF Sco Min II 13.8.
CK Sco VB A (B 15m, 14").
CL Sco The brightness in optical and UV ran-
ge is modulated according to the elements: Min (pg) =
= 2427020 + 624.7d*E.
Outbursts 1892, 1899, 1907, 1926.
CP Sco N /= 4.
CQ Sco [A/H] = -1.4.
DX Sco VB A (B p).
EZ Sco VB A (B 15.6m nf).
FQ Sco VB A (B 16m vis).
FU Sco VB A (B np).
Min II 12.7, Min II - MiN I = 0.493P.
FV Sco d = 0.015P. Depth of Min II 0.1m pg.
FY Sco VB A (B 15m, 15", 35deg).
GG Sco VB A (B 15m, 8", 45deg).
GM Sco The nothern one of the two stars noted
on the chart for SVS 1677.
GW Sco VB A (B = BI Sco, 6", 150deg).
IU Sco VB A (B 16.4m nf).
Max = 2413280 + 69.05d*E (1893 - 1906);
during 1910 - 1928 - see
Table.
KO Sco Rapid variations: A = 1.0m.
Slow changes:
A = 0.5m, P = 2000d +-.
KQ Sco [A/H] = + 0.3. P var?
LO Sco P var? Before JD2419150 Max = 2411500 + 450d*E;
since JD2423900 - see Table.
The spectrum is later than M5.
LR Sco The spectrum resembles RCrB in Max light [8090].
IR excess. RCB type minima were not observed.
OO Sco In the region of
the open cluster TR 29.
QZ Sco P var. Before JD2420400 Max = 2412640 + 158d*E;
since JD2423900 - see Table.
V347 Sco P var. Before JD2418700 Max = 2411500 + 198d*E;
since JD2423900 - see Table.
V381 Sco d = 0.046P.
V382 Sco See SY Sco.
V385 Sco In the region of
the open cluster CR 338.
V387 Sco Min II 12.2.
V390 Sco P var. Before JD2422500 Max = 2420330 + 466d*E;
since JD2423900 - see Table.
V393 Sco Min II 8.3.
V400 Sco Min II 15.0.
V402 Sco See SY Sco.
V403 Sco d ~ 0.02P. The depth of Min II 0.05m.
V407 Sco See SY Sco.
V411 Sco Min II 14.0.
V412 Sco Min II 14.8. See SY Sco.
V420 Sco See SY Sco.
V421 Sco P var. Before JD2418000 Max = 2413830 + 293d*E;
since JD2423900 - see Table.
V423 Sco Min II 14.2. See SY Sco.
V425 - V426 Sco
See SY Sco.
V429 Sco See SY Sco.
V430 Sco In the region of
the open cluster Tr 30.
V432 Sco See V430 Sco.
V437 Sco d = 0.02P. Min II 13.9.
V438 Sco Positions of the variable in the charts
[0021] And [6286] differ.
V439 Sco P var. Before JD2418200 Max = 2413350 + 166.5d*E;
since JD2419900 - see Table.
V440 Sco See V430 Sco.
V446 Sco P var? before JD2435000 Max = 2434980.1 +
+ 28.6195d. [A/H] = -1.0.
V450 Sco A = 0.9m pg.
V453 Sco VB A (B 13.51m, F7V, 13.5", 168deg). Min II 6.70.
The light curve shape var?
V455 Sco P.K.351deg + 3deg1. Planetary nebula natu-
re is doubtful. Nova-like outbursts separated by se-
veral years.
V457 Sco Min II 11.3.
V460 Sco d = 0.02P.
V464 Sco d = 0.03P.
V466 Sco Min II 13.7.
V467 Sco P var. P = 2.41354d (1889 - 1903); since 1903 -
see Table.
V470 Sco [A/H] = 0.1.
V471 Sco Min II 15.2, dII = 0.08P(!).
V472 Sco d = 0.02P.
V474 Sco Min II 10.6.
V483 Sco CI = +3.5m.
V485 Sco Short term variations are superimposed.
V486 Sco D >= 4d? P = 1d is possible.
In the region of
the open cluster NGC 6383.
V487 Sco [Fe/H] = -1.67, delta(S) = 9.0.
V490 Sco Min II 12.5.
V491 Sco Min II 13.2.
V494 Sco A var (1.27m - 1.66m B). P var? delta(S) = 2.
VB A (B 12.72m y, 23").
V495 Sco See V485 Sco (delta(m)short = 0.5m +-).
V496 Sco In the region of
the open cluster NGC 6414.
d = 0.03P.
V497 Sco Min II 13.6.
V499 Sco AII = 0.47m V. Min I - Min II = 0.504P.
V502 Sco In the region of
the open cluster C 1712 - 407.
V507 Sco The epoch of Max from [0300] contradicts the ele-
ments.
V540 Sco VB A (B 15.2m sp).
V547 Sco VB B (A 14.2m sf).
V549 Sco [A/H] = -1.1.
V555 Sco [A/H] = -0.3.
V562 Sco Min II 12.1.
V566 Sco d = 0.01P:.
V567 Sco VB A (B 13.01m, 10"sp, CD 30"nf). P var.
V568 Sco d = 0.04P.
V569 Sco Min II 11.4.
V570 Sco P var?
Unusually broad Max.
V573 Sco d = 0.06P. See V574 Sco.
V574 Sco In the region of
the open cluster Tr 24.
V575 Sco Min II 12.4.
V579 Sco See V574 Sco.
V581 Sco Min II 11.9.
V584 Sco Min II 13.1.
V585 Sco d = 0.03P:.
V586 Sco d = 0.04P. See V574 Sco.
V588 Sco d = 0.02P. See V574 Sco.
V589 Sco d = 0.05P. See V574 Sco.
V590 Sco In the region of
the open cluster NGC 6231.
V592 Sco Min II 13.3.
V593 Sco d = 0.05P:.
V594 Sco d = 0.01P.
V603 Sco d = 0.04P.
V606 Sco d = 0.07P.
V607 Sco Min II 10.3.
V609 Sco Min II 13.7.
V611 Sco d = 0.04P. Min II 13.7.
V612 Sco d = 0.05P.
V613 Sco d = 0.04P.
V616 Sco Min II 12.4.
V619 Sco Min II 12.1.
V620 Sco d = 0.02P.
V621 Sco d = 0.04P.
V622 Sco Min II 14.2.
V623 Sco Long intervals in Max without
changes, sometimes becomes faint.
V625 Sco VB A (B 13.2m sf). Min II 13.5.
V627 Sco Min II 14.1.
V628 Sco Min II 12.4.
V629 Sco Apsidal motion.
V631 Sco Min II 13.2.
V632 Sco d = 0.06P.
V633 Sco Min II 12.2.
V634 Sco Min II 12.2.
V636 Sco SB1 (Porb = 1318d).
V638 Sco d = 0.07P.
V640 Sco Min II 13.5.
V660 Sco VB A (B 16.0m s).
V672 Sco P = 180d is possible.
V674 Sco VB A (B 15.0m s).
V679 Sco P = 364d is possible.
V690 Sco VB A (B 14.40m y, 6", 0deg).
The range of the combined light is given.
delta(S) = 4.
V698 Sco D <= 0.20d, d = 0.043d.
V700 Sco Min II 10.3.
V701 Sco Min II 9.05. P var. Min I = 2439329.6657 + 0.76187133d*E
(JD2428000 - 39400) [7177]; since
JD2439400 - see Table.
See V702 Sco.
V702 Sco Probable
member of the open cluster NGC 6383.
V703 Sco P0 = 0.1499615d [3521]; P1 - see Table
(P var?). Also noted P =
= 0.04162025d [3521]. A var (0.23m - 0.46m).
Beat phenomenon: Max = 2436760.249 +
+ 0.497306d*E [3521]. delta(S) = 1.
See BM Sco.
V705 Sco Min II 14.1:.
V706 Sco Moments of Max from [0046] contradict the
tabulated elements. According to [4678], A <= 0.05m V
during 6 nights.
V708 Sco See SY Sco.
V709 Sco See SY Sco. [A/H] = -0.6.
V710 Sco Min II 14.2.
V711 Sco See SY Sco.
V712 Sco Min II 14.0.
V714 Sco d = 0.05P:. See V732 Sco.
V717 Sco [A/H] = 0.9.
V718 Sco D ~ 4d. Another Min 2429847 - 849 [0270].
V720 Sco See SY Sco.
V723 Sco See SY Sco. At the
edge of a dark cloud.
V725 Sco VB B (A = AU Sco, B 0.4', 0deg).
V729 Sco Possibly a Nova.
V732 Sco P may be twice longer.
V733 - V734 Sco
See V729 Sco.
V735 Sco The light curve
shape var.
V738 Sco d = 0.04P:; Min II 13.4:. See SY Sco.
V740 Sco See SY Sco.
V749 Sco P = 410d is possible.
V756 Sco Min II 10.7.
V760 SCP dI = 0.02P; Min II 7.4; DII = 0.2P:, dII = 0.03P.
V761 Sco IN type is not excluded.
V764 Sco Min II 9.0.
V805 Sco Possibly P is twice
shorter.
V818 Sco Sco X-1. SB.
Var X-ray and multi-component radio sour-
ce. Lx/Lbol = 300 - 1000. The epoch of Min is
given for the periodic component of the light variati-
on (A ~ 0.25m). Flickering and flares up to 1m with
time scale from dozens of seconds to minutes. The
mean brightness level decreased in the middle of
1960-es by 0.3m-0.4m. The spectrum with blue conti-
nuum and H, HeI, HeII, CIII, NIII emissions.
V819 Sco Min II 13.2.
V821 Sco Min II 14.5.
V822 Sco VB? Combined brightness.
V827 Sco Min II 14.1.
V833 Sco Min II 11.2.
V837 Sco d ~ 0.03P:; Min II 14.3.
V838 Sco Min II 13.4.
V842 Sco Min II 12.3.
V843 Sco Min II 10.5.
V848 Sco Min II 13.1. RRC type with twice shorter period is possib-
le.
V849 Sco Min II 14.1.
V853 Sco d = 0.05P; Min II 14.1.
V856 Sco VB C (A = BS 6000, 6.65m, AO-3III; B 12.55m, 16",
298deg; C 44", 185deg; D 11.7m, CD 1.3", 105deg, 1945).
V857 Sco Erroneously labelled "10" (instead of "11") in the
chart.
V858 Sco Erroneously labelled "11" (instead of "10") in the
chart.
V861 Sco SB1. Min II 6.28. Depths of minima var.
In the region of
open cluster NGC 6231, Cr 316, Tr 24.
V862 Sco Usually 6.67m - 6.76m.
A flare of 40m duration on July 3, 1965.
See BM Sco.
V866 Sco VB (delta(m) ~ 0.5m, ~ 1", 200deg). m (6370 A) =
11.14m - 12.37m.
IR excess.
V870 Sco B-V = +3.38m - +3.52m. See V590 Sco.
V877 Sco Min II 13.1.
V883 Sco VB A (B 12.60m, 9", 130deg). P var?
Min = 2438228.315 + 1.294745d*E (JD2438200 - 40500)
[6871]; since JD2440500 - see
Table.
Deep Min II.
V884 Sco 4U 1700-37. LX/Lbol = 0.00007.
Eclipsing X-ray source. Eclipse duration is variable
in the ranges 0.61d <= dx <= 1.10d. The epoch of the midd-
le of the X-ray eclipse coinciding with Min II is gi-
ven. X-ray flux var in the scale from seconds till
hours. Sometimes a periodic modulation with P ~ 97
Min is present, its amplitude in the optical bAnd rea-
ches delta(V) ~ 0.01m.
Min II 6.57; Min I - Min II = 0.63P, dI=0.2P.
Surrounded by the ring nebula sh 2. in the region of
the open cluster NGC 6281. Field star.
V885 Sco Noticeable Min II.
V889 Sco The nortHern compo-
nent of a triple.
V890 Sco VB A (B 11.5m, 0.5' n).
V894 Sco A = 0.6m pg.
V896 Sco Co-ordinates or the chart may be erroneous.
V900 Sco See V590 Sco.
The light curve is a sinusoidal wave. Possib-
ly P = 6.20d; 6.85d.
V903 Sco N96 [2448]. Erroneously
identified with V479 Sco.
V906 Sco See SY Sco. Probab-
le cluster member. VB (delta(mV) = 0.8m, 0.1", 111deg, 1957).
The range of the combined light variation is given.
Min II 6.21.
V907 Sco See SY Sco. Min II 9.2.
V911 Sco Alternative P = 4.2d.
V913 Sco Alternative P = 0.976d.
IR excess.
V914 Sco VB (delta(mV) = 2m, 3", 200deg).
Sine wave with P = 2.69d,
delta(B) = 0.15m (B = 12.91m) [9753].
V915 Sco VB A (B 10.43m, WN6, 14", 330deg; C 11.40m, 20", 202deg;
D 13.96m, 22", 80deg, 1973).
The brightness decreased from 6.32m to 6.50m during
JD2443680 - 44115.
V917 Sco VB A (B 17m: sp).
The out-
burst: rise 1930-1936, Max 1936-1938, decline
1938-1952.
V919 Sco See V590 Sco.
V920 Sco See V590 Sco.
Multiple periodici-
ty: P1 - see Table, semi-
amplitude A1 = 0.0051m; P2 = 0.10765d. A2 = 0.0046m;
P3 = 0.10388d, A3 = 0.00485m; P4 = 0.12137d, A4 =
= 0.0036m; P5 = 0.6929d?, A5 = 0.0028m.
V921 Sco The star illuminates
a nebula.
V922 Sco Multiple pe-
riodicity, superposition of frequencies with amplitudes
0.0010m - 0.0352m.
V923 Sco D = 0.32d:.
The elements need confirmation.
In the region of
the open cluster NGC 6281.
V924 Sco B-V var: +1.90, +2.50,
Light fluctuations by 0.1m - 0.2m (u, b) in several
minutes.
V925 Sco VB A (B ~ 10", faint, blue).
Probable member
of the open cluster TR 27.
In Vr possible values
of P: 105.3d, 73.0d, 188.7d, 312.5d [9950].
V926 Sco 3U 1735-44 = Sco XR-3.
Bursts
superimpose small light variations with P = 0.18d
which is apparently the orbital period [4394].
V927 Sco The epoch
of Min in U light is given. IR excess.
alf Sco ADS 10074 A(B 5.1m, B4Ve, A = 2.9", Porb = 878 yr.).
Connected with a nebula.
zet 1 Sco
See V590 Sco.
kap Sco SB. P2 = 0.205430d. P1 var. Beat phenomenon:
Pi = 7.3316d.
lam Sco SB 1. Porb = 5.6d? Apuls = 0.02m.
Long period light changes:
Max = 2440376.15 + 10.1605d*E [9761].
One eclipse was found (JD2440690,
A ~ 0.04m) [6388].
mu 1 Sco Min II 3.12.
sig Sco VB AA (A 5.5m, 0.37", 96deg, 1981,
orbital motion?; B 8.45m, B9.5V, 20.1", 273deg,
1961); SB1, Porb = 33.06d. P0 var.
Max Vr = 2420000.1465 + 0.24682815d*E (1918 - 1924)
[9953]; Max = 2432306.918 + 0.246846d*E (JD
2432000 - 37800) [9764]; since JD2437800 -
see Table.
A0 = 0.036m y. P1 = 0.2396674d, A1 = 0.013m y [9762].
Pbeat = 8.256d = Porb/4 [9957].
Connected with a nebula.
R Scl VB A (B 19.9m, 10", 234deg). CO emission.
S Scl P var. Max = 412774 + 367.9d*E (JD2405400 - 20500);
Max = 2423035 + 360.6d*E (JD2421250 - 27740);
Max = 2427738 + 370.4d*E (JD2427700 - 34000) [0960];
Since JD2434000 - see Table.
H2O emission.
T Scl P var. Max = 2417400 + 202.26d*E (JD2411300 -
19000); Max = 2420390 + 197.85d*E (JD2419000 -
23600); since JD2423600 - see
Table.
V Scl P var. Max = 2414006 + 294.8d*E (JD2411600 - 18200);
Max = 2422866 + 297.2d*E (JD2420400 - 35100);
since JD2435100 - see Table.
X Scl P var. Max = 2413796 + 258.7d*E (JD2413500 - 22800);
since JD2422800 - see Table.
Y Scl The cycles 100d: and 300d: are sometimes observed.
RT Scl Min II 10.47. [Fe/H] = -0.75. P var.
There is
a nonlinear term in the elements given in the Table:
-9.04d*10**-11*E**2.
RU Scl (k - b)2 = 0.09. A var [3429]. P var. Max = 2425094.4175 +
+ 0.4933257d*E (JD2416750 - 25100) [0183]; Max =
= 2427403.177 + 0.4933239d*E (JD2425100 - 30650)
[1381]; since JD2430650 - see
Table.
RW Scl P var?
SV Scl [Fe/H] = -1.82. P var? Max = 2439468.364 +
+ 0.3773636d*E (JD2427300 - 39500) [5233];
since JD2439850 - see Table.
SY Scl H2O maser.
P var? Max = 2426160 + 411d*E [0193]; since
JD2440400 - see Table.
SZ Scl Min II 13.68.
UY Scl Near the galaxy NGC 55.
UZ Scl VB A (B 15.81m, 23", 135deg); (k - b)2 = 0.14. See
V818 Sgr.
VV Scl Min II 8.50. ACV? [8083].
VY Scl Porb = 0.1662d? [9932].
High and low states of the
system are observed.
VZ Scl High and low states of the system are observed
[9933].
WZ Scl THere are two oscillations with the periods P1 and
P2: P1 = 0.06576d, P2 = 0.095944d, P1/P2 = 0.6854.
XX Scl There are two oscillations with the periods P1 and
P2: P1 = 0.048898d, P2 = 0.051350d, P1/P2 = 0.95225.
AI Scl There are two oscillations with the periods P1 and
P2: P1 = 0.044d, P2 = 0.0931d, P1/P2 = 0.47.
AL Scl Min II 6.20; Min II - Min I = 0.475P; DII = 0.08P.
AO Scl mu = 0.46", P = 187deg.
R Sct [Fe/H] = -1. P var. Min I = 2377165 + 142.8d*E
(JD2377160 - 9820); Min I = 2384885 + 142.6d*E
(JD2384890 - 8170); Min I = 2394451 + 141.4d*E
(JD2394450 - 8500); Min I = 2398777 + 142.4d*E
(JD2398770 - 2404320); Min I = 2404627 + 137.4d*E
(JD2404600 - 6410); Min I = 2406561 + 142.7d*E
(JD2406560 - 9065); Min I = 2409742 + 143.6d*E
(JD2409730 - 12700); Min I = 2412755 + 141.5d*E
(JD2412750 - 16720); Min I = 2417161 + 139.5d*E
(JD2417150 - 20790); Min I = 2421083 + 143.4d*E
(JD2421050 - 25170) [9935]; Min I = 2429478 + 142.8d*E
(JD2429000 - 30650) [9938]; Min I = 2432078 + 140.05d*E
(JD2432000 - 42240) [7596]; Min I = 2442737 + 152.5d*E
(JD2442550 - 43050); Min I = 2443315 + 138.5d*E
(JD2443050 - 44150) [0001]; since
JD2444150 - see Table.
Light curve drawings [9935,
9936, 9937].
Spectrum description [9939, 9954].
S Sct VB A (B 11.9M V, 14.5", 238deg; C 12.5m V, 44", 105deg).
U Sct Min II 10.31.
W Sct Min II 10.1.
X Sct [A/H] = -0.1. In the
region of the open cluster NGC 6639.
Y Sct In the region of the
open cluster NGC 6664.
Z Sct [A/H] = 0.3.
RS Sct Min II 10.08.
RU Sct [A/H] = -0.7. P var.
There is a nonline-
ar term in the elements given in the Table:
+3.15d*10**-6*E**2.
RX Sct Connec-
ted with the bright hydrogen nebula YM 13.
RY Sct Min II 9.56. P var? Min I = 2427979.340 + 11.124939d*E
(JD2414800 - 36100) [0007]; since
JD2431200 - see Table.
The shape of the
light curve varies.
RZ Sct Min II 7.47. P var.
There is nonline-
ar term in the elements given in the Table:
+ 0.78d*10**-7*E**2.
SU Sct P var. Max = 2424324.48 + 1.467713d*E (JD2420700 -
34310); Max = 2439678.428 + 1.468753d*E
(JD2437100 - 41100) [7806]; since
JD2441100 - see Table.
TX Sct CWA? red.
TY Sct [A/H] = -0.3. In the
region of the open cluster Tr 35.
UZ Sct [Fe/H] = 0.35. P var. Max = 2435629.5 + 14.7468d*E
(JD2423900 - 35700) [2309]; since JD
2436000 - see Table.
VV Sct SF component of a
pair.
VW Sct P var. Max = 2415887 + 234d*E (JD2411900 - 22210);
Max = 2423588 + 235d*E (JD2422880 - 27600);
Max = 2429468 + 235.1d*E (JD2428750 - 34200);
since JD2434600 - see Table.
VX Sct d = 0.064P.
VZ Sct Min II 12.0.
WY Sct P var.
XY Sct Min II 14.5.
AC Sct d = 0.024P; Min II 10.2.
AE Sct d = 0.04P.
AI Sct In the region of the
open cluster NGC 6705.
AN Sct P var?
AP Sct V2 (NGC 6712).
AU Sct d ~ 0.03P.
BC Sct Following component of a
close double system. The companion - NSV 11551.
BH Sct Min II 14.9.
BI Sct VB A (B 16.3m:, 3", 280deg; C 16.7m:, 12", 190deg;
D 16.8m:, 18", 45deg; E 17.0m:, 6", 350deg).
BK Sct Close companion 16.5m sf.
BN Sct d = 0.02P.
BP Sct S 5.5/5.5.
BS Sct Min II 11.07. In the
region of the open cluster M11 (NGC 6705).
BU Sct A var. P var. Max = 2425804.625 + 0.42022d*E [1401];
Max = 2427928.041 + 0.4202188d*E (JD2427900 -
9440) [1404]; Max = 2432770.464 + 0.4201944d*E
(JD2432740 - 38290); Max = 2438589.357 +
+ 0.4202171d*E (JD2438580 - 40510) [7806];
since JD2440770 - see Table.
BX Sct [A/H] = -0.9.
CD Sct Min II 13.7.
CF Sct d = 0.035P.
CH Sct V7 (NGC 6712).
The member of this globular cluster.
CK Sct [Fe/H] = 0.23.
CL Sct May be the
period should be doubled?
CM Sct [A/H] = 0.1.
CN Sct [A/H] = -1.5.
CO Sct P var? Resembles RV Tau type
variables: if the period is doubled, the neight of
max I And the depth of Min II vary.
CR Sct Min II 12.1; DII = 0.071P; Min II - Min I = 0.53P.
CT Sct Min II 11.1.
CW Sct Min II 10.1.
CZ Sct See V1389 Sgr.
DD Sct One of the components probably varies.
DE Sct Min II 16.3.
DG Sct d = 0.03P:.
DL Sct Min II 15.9.
DT Sct Min II 16.5.
DV Sct Min II 17.8.
DW Sct Min II 16.4.
EE Sct Min II 15.3.
EH Sct Min II 15.0.
EK Sct Min II 16.0.
EL Sct The shape of the
light curve varies?
EN Sct Min II 17.2.
The different elements are also possible:
Min I = 2428008.85 + 1.06446d*E.
EP Sct d = 0.04P:; Min II 15.6.
EQ Sct In the region of
the open cluster NGC 6631.
Min II 12.6:.
ER Sct Min II 9.3; Min II - Min I = 0.506P; DII = 0.14P.
EU Sct VB A (B 17.5m, 6", 45deg).
EV Sct [A/H] = -0.4. The mem-
ber of the open cluster NGC 6664.
EW Sct P0 = 5.8195d (A/2 = 0.27m), P1 = 4.0646d (A/2 = 0.22m);
P1/P0 = 0.6984.
EX Sct d = 0.025P:.
EY Sct Min II 12.4. In
the region of the open cluster NGC 6683.
EZ Sct Min II 12.5.
FF Sct Min II 14.2.
FG Sct Min II 14.70. P var? Min I = 2429017.557 +
+ 0.2705728d*E (JD2427975 - 29520) [1397];
since JD2444700 - see Table.
FH Sct In the region of
the open cluster NGC 6694.
FK Sct Min II 14.4:.
FL Sct Min II 13.8.
FM Sct Min II 12.9.
FN Sct In the open cluster
NGC 6704.
FO Sct D = 0.22d.
FR Sct Spectrum description [1410].
GI Sct Min II 14.5.
GM Sct Min II 13.8:.
HI Sct D = 0.29d.
HL Sct Min II 13.4.
IS Sct P < 200d.
IT Sct In the region of
the open cluster NGC 6705.
LL Sct sf compo-
nent of a close pair.
LR Sct In the region of the
globular cluster NGC 6712.
LU Sct P2 = 30d.
LZ Sct See LR Sct.
MM Sct Min II 15.8.
MP Sct V1 (NGC 6712).
The member of this globular cluster.
[Fe/H] = -0.69.
MR Sct V8 (NGC 6712). P var. Max = 2430885 + 117d*E
(JD2427900 - 32400) [4231]; since
JD2434900 - see Table.
NU Sct VB A (B 16.6m, 12", 180deg).
NV Sct P = 200d?
OU Sct P var. Max = 2427620 + 152d*E (JD2426200 - 32800);
since JD2433100 - see Table.
PT Sct There is a close
companion, 16.4m.
PW Sct The range of the combined light of the variable and
a close companion, which follows, is given in the
Table.
QU Sct The variable is also eclipsing one with
P = 0.2d and A = 0.7m.
V337 Sct A close companion (16.2m, <7",
90deg).
V340 Sct Min II 15.6.
V356 Sct Min II 12.3; DII = 0.10P.
V360 Sct A close fn companion,
16.4m.
V362 Sct P = 170d?
V367 Sct In the open cluster
NGC 6649.
The light elements
with fundamental mode period P0 (A0 = 0.54m B) are
given in the Table. For the first-overtone period
P1 (A1 = 0.41m B) Max = 2437435.12 + 4.38466d*E;
P1/P0 = 0.696744.
M - m var (0.15 <= M - m <= 0.45).
V369 Sct In the region of
the open cluster NGC 6705 (M 11).
THere is a superposition of the four
light oscillations: P1 = 0.240d (A1 = 0.044m), P2 = 0.220d
(A2 = 0.020m), P3 = 0.182d (A3 = 0.068m), P4 = 0.114d
(A4 = 0.028m) [9745].
V370 Sct d = 0.016P.
V372 Sct d = 0.012P.
V414 Sct Blue companion?
del Sct VB A (B 10m, 53", 130deg); (k - b)2 = 0.37.
The basic light variation P0 (A0 = 0.125m) given in the
Table is superposed by the secondary one with P1 =
0.1867756 (A1 = 0.034) [9975].
R Ser P var. Max = 2372429 + 356.93d*E (JD2372400 -
88900) [0960]; Max = 2397809 + 353.00d*E
(JD2394000 - 2403000); Max = 2403104 + 357.25d*E
(JD2403000 - 24000); Max = 2432387 + 356.10D*E
(JD2424000-39200); since JD2441000 -
see Table.
Maser (SiO, H2O).
S Ser P var. Max = 2394360 + 361.01d*E (JD2394000 -
2407000); Max = 2407024 + 372.70d*E (JD2407000 -
17000) [0960]; Max = 2425875 + 366.59d*E
(JD2417000 - 36000); since JD2437600 -
see Table.
Maser (OH, SiO, H2O).
T Ser In the region of
the open cluster NGC 6633.
P var. Max = 2400907 + 342.05d*E (JD2400500 -
15000); Max = 2417912 + 345.73d*E (JD2417900 -
26000); Max = 2428524 + 332.21d*E (JD2426000 -
32500); Max = 2438382 + 345.71d*E (JD2432500 -
39500); since JD2439500 - see
Table.
0.8' from BN Ser.
U Ser P var. Max = 2421158 + 237.70d*E (JD2414000 -
22000); Max = 2422347 + 236.78d*E (JD2422000 -
26600); Max = 2426609 + 239.21d*E (JD2426600 -
32500); since JD2432500 - see
Table.
V Ser Min II 9.85.
W Ser P var, nonlinear terms:
+ (3.140d*10**-6)*E**2 + (1.432d*10**-9)*E**3.
The light curve shape var. Wave-
like variations in Max light. Changes of emission
lines with the orbital phase. Active mass exchange,
evidence for a common envelope.
X Ser After 1932 variations 14.3m - 18.3m were no-
ted; according to [1417], P = 275d. Observations in
1961 - 1964 did not confirm P = 275d, fluctuations of
light with a period of several minutes were suspected
[3625].
The
spectral data are for 1981.
Y Ser Epoch of min is
given. According to [8643], variations with P ~ 400d
are superimposed by P ~ 40d.
Z Ser The elements are
valid during JD2422000 - 31000.
RS Ser Min II 11.4.
RT Ser Max (1920 - 1923).
In the spectrum
(1977 - 1979) there are emissions H alfa - H delta, HeI, HeII,
[OI] etc. Absorptions TiO.
RV Ser Maser (H2O).
VY Ser [Fe/H] = -1.77, delta(S) = 9.
WW Ser Maser (H2O).
WX Ser Maser (OH, SiO, H2O). P var?
AA Ser [A/H] = 0.2.
AG Ser P var? since JD2435000 - see
Table.
AK Ser P var? before JD2442300 Min = 2431313.266 +
+ 1.9225667d*E [0318]; since JD2442300 -
see Table.
AN Ser P var? Max = 2429156.260 + 0.5220703d*E
(JD2427000 - 38000) [0001]; since
JD2438000 - see Table.
According to [2740], Blazhko effect with Pi = 21.94d;
the presence of the Blazhko effect is denied in
[7258].
delta(S) = 0.
AO Ser Min II 10.8.
AP Ser VB A (B 14.29m, 8" sp). [Fe/H] = -1.37.
AQ Ser Min II 11.1.
AR Ser P var. Before JD2425000 Max = 2415617.698 +
+ 0.5752221d*E; Max = 2425313.530 + 0.57508945d*E
(JD2425000 - 28500); Max = 2428848.662 +
+ 0.575214d*E (JD2428500 - 31000) [8081]; Max =
= 2431436.424 + 0.5751134d*E (JD2431000 - 34200);
Max = 2436013.279 + 0.5752169d*E (JD2435900 -
37200); Max = 2438138.467 + 0.5750651d*E
(JD2437200 - 38700) [0001].
Elements working on average since
JD2438700 - see Table.
Complex Blazhko effect.
Pi = 108.4d [8082]. A var (0.23m - 0.87m V). Pi var (80d -
120d) [7032].
delta(S) = 4.6.
AS Ser Min II 11.5.
The epoch of Min I 2442937.428
(BBSAG) is not in agreement with the elements.
AT Ser P var. Max = 2415353.783 + 0.74655695d*E
(JD2415000 - 27000); Max = 2428337.260 +
+ 0.7465670d*E (JD2428000 - 39500); since
JD2441500 - see Table.
delta(S) = 9.
AU Ser Min II 11.61.
The light curve shape var.
AV Ser delta(S) = 6.
AW Ser delta(S) = 5.0.
BF Ser [A/H] = -2.5. delta(S) = 6.
BH Ser P var. Max = 2427956.674 + 0.434545d*E (JD2425000 -
30700) [1039]; since JD2437650 -
See Table.
BI Ser Min I 2446264.414 [10200]
contradicts the elements. P var?
BN Ser In the region of
the open cluster NGC 6633. 0.8' From T Ser.
BO Ser P var? Max = 2425681 + 201d (JD2425600 - 30100)
[0447]; the
Table gives mean elements (JD2425600 - 35400).
BQ Ser P0 - see Table. P1 = 3.012d [8188].
see BR Ser.
BR - BU Ser
In the region
of the open cluster IC 4756.
CC Ser Min II 11.63.
CN Ser [Fe/H] = -0.77. delta(S) = 3.4.
CO Ser P var? The light curve shape
var.
[Fe/H] = -1.38. delta(S) = 7.2.
CQ Ser Min II 12.0.
CR Ser [A/H] = -0.2.
CS Ser P var. Max = 2418137.875 + 0.5267904d*E
(JD2416000 - 32500) [0001]; since
JD2432500 - see Table.
delta(S) = (6).
In the region of the HII complex S 54 and the open
star cluster NGC 6604. Connected with a shell-struc-
ture nebula.
Sometimes eclipses are observed during the configu-
ration "WR in front of O" (see Table) and sometimes
during the configuration "O in front of WR" which
coincided with the deepest eclipse ever observed
(with the depth 0.5m B, V). Sometimes the photomet-
ric eclipse at predicted moments does not occur, and
only the atmospheric eclipse of the O star with the
WR component is observed at lambda 4653 A (emission of
CII - CIV, NIII), lambda < 2000 A. IR excess; possibly an
IR eclipse in the configuration "O in front of WR".
CX Ser The light curve (resembling the eclip-
sing light curve of U Gem) shows a hump of ~ 0.2m
height before the minimum; fluctuations up to ~ 0.3m -
0.4m in Max.
DF Ser VB A (B 13.9m, 0.4', -115deg).
DG Ser Min II 16.5:. The
alias period is possible (0.3360742d).
DH Ser AnotHer possible P = 450d.
DK Ser Max 2433829 [10008]
Contradicts the elements.
DR Ser VB A (B 12.54m, 28", 0deg).
DT Ser VB A (B ~ 5").
The spectrum shows emissions
of [OIII] lambda lambda 4959, 5007 A. O-
Symbiotic? [8676].
DV Ser In a small star
cluster.
DY Ser [Fe/H] = -1.58. delta(S) = 8.4.
EE - EF Ser
In the region
of the open cluster M 17 = NGC 6618.
EG Ser VB A (ro > 10").
EL Ser N <= 7.
EN Ser [Fe/H] = -1.07. delta(S) = 5.3.
EO Ser The light curve shows large scatter. RR(B)
type is possible.
Max = 2437433.653 + 0.6309d*E (JD2437433 - 514)
[3625].
[Fe/H] = -1.63. delta(S) = 8.8.
ER - ET Ser
In the regi-
on of the open cluster M 16 = NGC 6611.
EU Ser VB A (B 4" np).
A member of the open cluster M 16 = NGC 6611.
IR excess.
EV - EX Ser
See ER Ser.
FI Ser Hints of
periodicity in U light.
FK Ser VB (delta(m) ~ 0.5m, 1.3", 11.5deg, 1972).
Flares
Were found in the satellite UV range [10013]. Diffe-
rences from typical by stars and probable "post-
T Tau" nature are noted [7260, 3866].
According to [6948], Min = 2441939.200 +
+ 5.20d*E.
Soft X-ray source.
FL Ser VB (delta(m) = 1.9m, 0.46", 145deg, 1981).
FM Ser See ER Ser.
VB (var sf?).
FN Ser See ER Ser.
FR Ser ADS 11477 A (B 12.5m, 10.5", 330deg, 1924; C 9.3m,
30.5", 5deg, 1930).
Possible values of P:
2.1308d, 2.1565d.
LN Ser m pg ~ 17.5m ~ const; blue compa-
nion? [7264].
LS Ser The light curve shows
Large scatter, the elements need confirmation.
Possible identification with an X-ray source
2ASE 1822 + 0.
LV Ser The epoch of max in V light is given;
in B and U varies in opposite phase.
LX Ser The depth of eclipses ~ 2.5m.
Comparatively fre-
quent outbursts [10023].
MM Ser Ser X-1 = 4 U 1 837 + 04. LX/Lopt >= 100.
VB B (A 19.1m; B 2.2", 210deg).
MO Ser V1 (NGC 6535). Cluster non-
member.
MP Ser V2 (NGC 6535). Cluster non-
member.
del Ser ADS 9701A (B 5.16m, dF0, a = 5.843", Porb = 3168 yr;
4", 175G, 1980).
omi Ser SB?
d Ser ADS 11353 A (B 7.44m, SB?, F5V, 3.9", 320deg, 1983).
VB (speckle-interfe-
rometric; 0.25", 157deg, 1976). SB (P1orb = 385d,
P2orb = 1.8505205d).
S Sex P var. Max = 2422029 + 257.2d*E (JD2417650 - 22050);
Max = 2428968 + 266.65d*E (JD2422050 - 30300); Max =
= 2434739 + 260.86d*E (JD2430300 - 34750); Max =
= 2438796 + 254.3d*E (JD2434750 - 38800);
since JD2440600 - see Table.
T Sex [Fe/H] = -1.20. P var. Max = 2416146.675 +
+ 0.32465971d*E (JD2414000 - 18300), Max =
= 2424561.398 + 0.32467107d*E (JD2418300 - 24570)
[0752]; Max = 2424561.430 + 0.3246702d*E
(JD2424560 - 28280), Max = 2429350.320 +
+ 0.3247113d*E (JD2429350 - 34370), Max =
= 2434795.409 + 0.3246978d*E (JD2434795 - 36630)
[9978]; since JD2441380 - see
Table.
U Sex P var. Max = 2419823.355 + 0.53402622d*E
(JD2419470 - 36670) [3697]; since
JD2443980 - see Table.
Y Sex Min II 10.17; dII = 0.05P. P var. Min I = 2428122.700 +
+ 0.41982341d*E (JD < 2429000) [0007]; Min I =
= 2434445.989 + 0.419818d*E (JD2428100 - 35000)
[0001], Min I = 2439521.964 + 0.41981543d*E
(JD2431150 - 43250) [9981]; since
JD2440300 - see Table.
RU Sex Min II 11.4. According to [9923], RR?
(P = 0.5398d?), CEP? (P = 6.792d?).
RW Sex Porb = 0.247d [9925]; LX/Lopt = 10**-4 [9926];
Px = 254s [9927].
RX Sex VB A (B 9.1m, 116.3", 191deg).
RY Sex Mu = 0.67", P = 281deg.
R Tau OH, H2O, Sio maser. P var. Max = 2411012 +
+ 325.0d*E (JD2398654 - 2414000); Max = 2424243 +
+ 322.1d*E (JD2414000 - 24300); Max = 2434005 +
+ 325.4d*E (JD2424300 - 35500); since
JD2435500 - see Table.
S Tau P var. Max = 2404646 + 380.1d*E (JD2399326 -
2405000); Max = 2425085 + 371.40d*E (JD2405000 -
26000); since JD2426000 - see
Table.
T Tau VB A (B 15m, 0.27", 358deg; C -
infrared companion, 0.590", 180deg).
Near the variable
nebula NGC 1555.
OH, H2O maser.
In the interval JD2402140 - 21000
the light range 9.3m - 13.5m,
since JD2421000 - only 9.5m - 10.8m.
U Tau VB (A 10.9m; B 12.0m, 3", 77deg).
V Tau P var. Max = 2417978 + 170.0d*E (JD2404550 - 18000);
Max = 2424580 + 169.3d*E (JD2418000 - 24600);
Max = 2432746 + 170.1d*E (JD2424600 - 33500);
Max = 2436970 + 168.7d*E (JD2433500 - 37300);
Max = 2442442 + 171.1d*E (JD2437300 - 43000);
since JD2443000 - see Table.
W Tau value is
given in the Table.
P var. Max = 2415320 + 274.1d*E (JD2410360 - 15500),
Max = 2421995 + 266.1d*E (JD2415500 - 22500),
Max = 2425135 + 260.5d*E (JD2422500 - 28800),
Max = 2438837 + 245.4d*E (JD2428800 - 39100) [0001].
Z Tau VB A (B 13.6m, 4", 45deg).
P var. Max = 2425115 + 499.90d*E (JD2415100 - 26500)
Max = 2438768 + 486.20d*E (JD2426500 - 39000);
since JD2439000 - see Table.
RR Tau Spectrum des-
cription and the photographs of the nebula [4002].
RU Tau VB A (B 4"). P var. Max = 2426004 + 545.3d*E
(JD2415009 - 27500). Max = 2434309 + 604.0d*E
(JD2427500 - 34500); since JD2437500 -
see Table.
RV Tau OH maser. Mean
brightness varies: Min = 2417553 + 1224d*E [0580].
RW Tau VB A (12.5m, 1.3", 172deg, 1959). dI = 0.020P; Min II 8.09.
P var. Min I = 2417198.410 + 2.7688665d*E +
+ 0.038d sin 0.0818deg (E - 100) (JD2409913 - 24150),
Min I = 2434423.3571 + 2.7688209d*E (JD2424150 -
37000) [5460]; Min I = 2437164.4860 + 2.7688480d*E
(JD2437000 - 39900) [7531]; Min I = 2442776.93772 +
+ 2.76884463d*E (JD2439855 - 42780) [8593]; Min I =
= 2442776.9313 + 2.7688396d*E (JD2442780 - 45750)
[9084]; since JD2445750 - see
Table.
The shape of the
light curve varies.
RX Tau OH, H2O maser.
P var. Max = 2423561 + 338.4d*E (JD2417155 - 24000);
Max = 2430505 + 330.2d*E (JD2424000 - 30700); Max =
= 2437963 + 339.3d*E (JD2430700 - 38000);
since JD2438000 - see Table.
RY Tau SB 1. The pho-
tographs of the nebula and spectrum description
[5064]. Long
period light variations are possible with cycles
70.25, 15.9, 9.4 and 5.84 years [9993].
RZ Tau Min II 10.66. P var. Min I = 2424032.1426 +
+ 0.41567109d*E (JD2424000 - 34100) [0312];
since JD2436000 - see Table.
SS Tau P var [3506]. Max = 2420894.2339 + 0.3699665d*E (JD
2420890 - 21300) [9995]; Max = 2426669.080 +
+ 0.3699687d*E (JD2426400 - 26700) [0320]; Max =
= 2428843.856 + 0.3699231d*E (JD2426700 - 30300),
Max = 2431392.603 + 0.369912d*E (JD2430300 - 31400),
Max = 2432118.794 + 0.369937d*E (JD2431400 - 32150),
Max = 2432857.884 + 0.3699146d*E (JD2432150 - 35000),
Max = 2435055.528 + 0.3699066d*E (JD2435000 - 36400),
Max = 2437313.503 + 0.3699266d*E (JD2436400 - 37320),
Max = 2437960.419 + 0.369878d*E (JD2437300 - 37960),
Max = 2437960.419 + 0.369938d*E (JD2437960 - 38740);
since JD2438740 - see Table.
SV Tau Min II 9.8.
SW Tau P var. Max = 2432049.856 + 1.583623d*E (JD2418240 -
36000); since JD2436000 - see
Table.
SX Tau In the region of the pleiades cluster. Not a member
of the cluster.
SY Tau See SX Tau.
SZ Tau The member
of the halo of the open cluster NGC 1647.
P var. Max = 2410000.60 + 3.1487d*E (JD2412000 -
20200) [9996]; Max = 2419267.519 + 3.149046d*E
(JD2419260 - 34650); since JD2434650 -
see Table.
TT Tau P = 364d? [0589].
TY Tau In the region of the hyades cluster. Not a member of
the cluster.
According to [9997], Min = 2422291.303 +
+ 0.539250d*E.
UU Tau See SX Tau.
UX Tau VB A (B 13.67m V, M2.5 VE, 5.74", 270.1deg, 1944).
UZ Tau VB A (B 15.16m B, M4VE (Li), 3.7", 271.5deg, 1944).
The range of the combined light variation is
given in the Table.
WW Tau P var. P = 114.8d (JD2414800 - 20800). P = 124.4d
(JD2420800 - 23700) [0634]; P = 114d (JD2424800 -
26300), P = 139d (JD2426300 - 27700) [0310]; P =
= 114d (JD2427900 - 30800), P = 131d (JD2430800 -
31500), P = 109d (JD2431500 - 33400) [0364];
since JD2433400 - see Table.
WY Tau Min II 11.73. P var? [10048].
WZ Tau VB.
XZ Tau VB A (B = HL Tau, 23", 273deg).
YZ Tau [Fe/H] = -1.53. See SX Tau.
There is a square term in the elements: -6d*10**-11*E**2.
AA Tau Cyclic light vari-
ation with P = 4.5d and 2d [10003] and also 8.2d [10004]
is possible.
AC Tau d = 0.025P. P var?
AH Tau Min II 11.85. P var? see SX Tau.
AL Tau P var. The depth of Min II 0.15m.
AM Tau d = 0.012P:. P var. Min I = 2427534.444 + 2.044018d*E
(JD2425580 - 27540), Min I = 2435019.436 +
+ 2.043935d*E (JD2433320 - 37020); since
JD2442365 - see Table.
AN Tau Min II 10.5; Min II - Min I = 0.53P. P var.
AP Tau Min II 14.7; Min II - Min I = 0.48P.
AS Tau P var. Min I = 2439390.595 + 3.4835542d*E (JD
2419440 - 44300) [7806]; since JD2444300 -
see Table.
AU Tau P var. Max = 2426642 + 71.0d*E (JD2426290 - 30400)
[0310]; since JD2438000 - see
Table.
AW Tau OH, H2O maser.
P var. Max = 2426278 + 690d*E (JD2416100 - 33850)
[0609]; since JD2433850 - see
Table.
BB Tau SC 7/7 e.
BK Tau See SX Tau.
BN Tau P var. Min I = 2435460.370 + 4.2542044d*E (JD
2419000-39100) [5466]; since JD2443000 -
see Table.
BP Tau There are quasisinusoidal light varia-
tions with P = 7.6d [10011].
BU Tau Pleione.
The member of the pleiades cluster.
BV Tau Min II 11.9.
BW Tau 3C 120. Seyfert galaxy;
Z = 0.033.
Spectrum description [10012].
CD Tau VB A (B 9.88m, 9.9", 148.8deg). Min II 7.31.
In the region of
the open cluster CR 65.
CF Tau d = 0.02P; Min II 10.2;
CH Tau See V1389 Sgr.
CM Tau SN 1054 in the Crab ne-
bula (NGC 1952 = M1); pulsar NP 0532.
The outburst epoch is JD2106210:.
The pulsed radiation varies precisely in phase over the who-
le spectrum, from radio waves to gamma rays with
P = 0.033S in the range 13.9m - 17.7m V. P var [10017, 10018]:
0.033095563927s (JD2440297.5094) <= P <= 0.033242051159s
(JD2444312.750).
CR Tau P = 1.362692d?
CT Tau Min II 11.12. P var. Min I = 2437312.369 + 0.6668274d*E
(JD2432700 - 38790) [10010]; since
JD2441400 - see Table.
CU Tau See SX Tau. Min II 11.90. P var. Min I =
= 2431822.5193 + 0.4126022d*E (JD2431060 - 2890)
[0604]; since JD2440960 - see
Table.
CZ Tau VB B (A = DD Tau; B 31", 13deg).
DD Tau VB A (B = CZ Tau; 31", 13deg.
DE Tau VB A (B 26", 10deg).
DG Tau Connected with a small bright arc-shaped ne-
bula.
DH Tau VB A (B = DI Tau, 16", 125deg).
According to [10004] there is
periodical light variability with P = 7.0d and A = 0.4m V.
DI Tau VB B (A = DH Tau; B 16", 125deg).
According to [10004] there is
periodical light variability with P ~ 7.0d and A < 0.4m V.
DL Tau VB A (B 17m V, 12", 333deg).
Cyclic
light variation with P = 2.7d is present [10003].
DN Tau THere are sinusoidal light variations with
P = 6.6d [10011].
DO Tau See DG Tau.
DS Tau VB A (B 13.7m, 4", 288deg).
Range of
Combined light variation of the pair is given in the
Table.
EI Tau VB?
EQ Tau Min II 10.97. See SX Tau.
ES Tau Min II 14.4; Min II - Min I = 0.52P; d = 0.005P.
ET Tau Min II 9.3.
EY Tau The member of the Hyades
cluster.
EZ Tau See EY Tau.
FH Tau See EY Tau.
FL Tau The member of the pleia-
des cluster.
FS Tau VB A (B 16", 289deg).
FV Tau VB A (B 13", 103deg).
FW Tau VB A (B 13", 243deg).
FY Tau VB B (A = FZ Tau, B 17", 250deg.)
FZ Tau VB A (B = FY Tau, 17", 250deg).
GG Tau VB A (B 18.5m, 12", 205deg).
GH Tau VB B (A = V807 Tau; B 21.4", 193deg).
GI Tau VB B (A = GK Tau; B 13", 329deg).
There are quasisinusoidal light variations with P =
= 7.2d [10011].
See DG Tau.
GK Tau VB A (B = GI Tau, 13", 329deg).
There
are quasisinusoidal light variations with P = 4.6d
[10011].
See DG Tau.
GL Tau The
central star of the planetary nebula PK 174 -14deg 1.
GP Tau P2 = 1000d.
GR Tau dI = 0.068P; Min II 10.49; Mim II - Min I = 0.516P.
GS Tau SB 1 (Porb = 7.227424d [6568]). See V1389 Sgr.
GU Tau VB A (B 11", 299deg).
GV Tau Herbug-haro object.
GW Tau Min II 11.7. P var?
GX Tau VB A (B 11", 310deg).
HK Tau VB A (B 21m, 2", 180deg).
HL Tau VB B (A = XZ Tau; B 23", 273deg). See DG Tau.
HN Tau VB A (B 18m, 3.3", 205deg).
HO Tau VB A (B 8", 110deg).
HP Tau See DG Tau.
According to [10004] there is pe-
riodical variability with P = 1.2d.
HR Tau VB B (A = HS Tau; B 14", 119deg).
HS Tau VB A (B = HR Tau; 14", 119deg).
HU Tau Min II 5.91.
HZ Tau In the region of the pleiades cluster. Possible
member of the cluster.
II Tau In the region of the pleiades cluster.
Possible member of the hyades cluster
IK Tau OH, H2O, SiO maser.
IM Tau P var. Max = 2439792.398 + 0.144969d*E (JD2439790 -
43130) [10019]; P1 = 0.109016d, P1/P0 = 0.752.
Since JD2444230 - see Table.
IN Tau mu = 0.121", P = 105deg. The mem-
ber of the hyades cluster?
IO Tau In the region of the hya-
des cluster.
IQ Tau VB A (B 17m, 11", 298deg).
IS Tau SVS 1319 [4051].
The star N23 with Halfa emission [0596]. In the map gi-
ven in [0596] erroneously designated as N26 in cont-
radiction with the co-ordinates given in the same pa-
per. It was the reason for different mistakes when the
star was identified by some other investigators.
IT Tau SVS 1320 [4051].
The star N26 with H alfa emission [0596].
See IS Tau.
KK Tau In the region of the
pleiades cluster.
KL - KO Tau
See KK Tau.
KP Tau See SX Tau.
KQ Tau See KK Tau.
KR Tau See SX Tau.
KS - KW Tau
See KK Tau.
KX Tau See SX Tau.
KY Tau See FL Tau.
KZ - LL Tau
See KK Tau.
LM Tau See HZ Tau.
LN Tau See KK Tau.
LO Tau See HZ Tau.
LP Tau See SX Tau.
LQ Tau See KK Tau.
LR Tau See II Tau.
LS Tau See KK Tau.
LT - LV Tau
See HZ Tau.
LW Tau See SX Tau.
LX Tau See KK Tau.
LY Tau See HZ Tau.
LZ - MM Tau
See FL Tau.
MN Tau See KK Tau.
MO Tau See HZ Tau.
MP - MQ Tau
See KK Tau.
MR - MS Tau
See FL Tau.
MT Tau See SX Tau.
MU - MV Tau
See HZ Tau.
MW Tau See KK Tau.
MX - MY Tau
See FL Tau.
MZ Tau See HZ Tau.
NN - NO Tau
See KK Tau.
NP Tau See FL Tau.
NQ Tau See KK Tau.
NR Tau See SX Tau.
NS Tau See KK Tau.
NT Tau See HZ Tau.
NU Tau See KK Tau.
NV Tau See SX Tau.
NW Tau See KK Tau.
NX - NY Tau
See SX Tau.
NZ - OO Tau
See KK Tau.
OP Tau See HZ Tau.
OQ Tau See KK Tau.
OR - OT Tau
See FL Tau.
OU Tau Max = 2444896.758 + 0.39701d*E, M - m = 0.5P, A(V) =
= 0.13m [10052].
See FL Tau.
OW Tau See FL Tau.
OX Tau See KK Tau.
OY Tau See SX Tau.
OZ - PP Tau
See HZ Tau.
PQ Tau See SX Tau.
PR Tau See FL Tau.
PS Tau See KK Tau.
PT Tau See FL Tau.
PU Tau See KK Tau.
PV Tau See HZ Tau.
PW - PZ Tau
See KK Tau.
QQ Tau SB2. See FL Tau.
QR - QT Tau
See KK Tau.
QU Tau VB A (B 18.0m, 4.0", 135deg). See KK Tau.
QV - QW Tau
See KK Tau.
QX Tau See FL Tau.
Max = 2444896.79 + 0.483d*E, M - m = 0.5P, A(V) = 0.125m
[10052].
QY Tau See SX Tau.
QZ - V335 Tau
See KK Tau.
V336 Tau See HZ Tau.
V337 Tau See KK Tau.
V338 Tau See HZ Tau.
V339 Tau See SX Tau.
V340 - V342 Tau
See KK Tau.
V343 Tau See FL Tau.
V344 - V345 Tau
See KK Tau.
V346 Tau See FL Tau.
V347 Tau See SX Tau.
V348 Tau See KK Tau.
V349 - V350 Tau
See HZ Tau.
V351 Tau See SX Tau.
V352 Tau See KK Tau.
V353 - V355 Tau
See HZ Tau.
V356 Tau See KK Tau.
V357 - V358 Tau
See FL Tau.
V359 - V360 Tau
See KK Tau.
V361 Tau See HZ Tau.
V362 Tau See KK Tau.
V363 - V364 Tau
See HZ Tau.
V365 Tau See KK Tau.
V366 Tau See FL Tau.
V367 - V369 Tau
See KK Tau.
V370 Tau See FL Tau.
V371 Tau VB (delta(m) ~ 1m, 1.5"). See FL Tau.
V372 Tau See FL Tau.
V373 - V374 Tau
See KK Tau.
V375 Tau See SX Tau.
V376 - V378 Tau
See FL Tau.
V379 - V380 Tau
See HZ Tau.
V381 - V382 Tau
See FL Tau.
V383 Tau See KK Tau.
V384 Tau See FL Tau.
V385 Tau See SX Tau.
V386 Tau TCSN 437. See KK Tau.
V387 - V388 Tau
See KK Tau.
V389 Tau TCSN 439. See KK Tau.
V390 Tau See KK Tau.
V392 Tau See HZ Tau.
V393 Tau See KK Tau.
V394 Tau See SX Tau.
V395 - V397 Tau
See KK Tau.
V398 Tau See HZ Tau.
V399 Tau See FL Tau.
V400 - V401 Tau
See KK Tau.
V402 - V403 Tau
See FL Tau.
V404 - V405 Tau
See KK Tau.
V410 Tau There are periodical light variations with P = 1.92d,
A(V) = 0.21m, M - m = 0.5P [10056].
V411 Tau mu = 0.13", P = 143deg.
Eruptive white dwarf. Usually there are quasi-perio-
dic variations with A ~ 0.3m and periods P0 = 12.436
Min and P1 = 8.237 Min (P1/P0 = 0.6624) which are
nonlinearly modulated by the third period PL ~ 0.135d
(probably by the orbital period of a faint companion).
V423 Tau Min II 15.8.
V425 Tau See SX Tau.
V426 - V429 Tau
See KK Tau.
V430 Tau See HZ Tau.
V431 - V434 Tau
See KK Tau.
V435 Tau See HZ Tau.
V436 - V437 Tau
See SX Tau.
V438 Tau See HZ Tau.
V439 - V440 Tau
See KK Tau.
V441 Tau See HZ Tau.
V442 - V443 Tau
See KK Tau.
V444 Tau See HZ Tau.
V445 Tau See KK Tau.
V446 Tau See FL Tau.
V447 Tau See SX Tau.
V448 Tau See FL Tau.
V449 Tau See SX Tau.
V451 Tau See SX Tau.
V452 - V453 Tau
See HZ Tau.
V454 Tau See SX Tau.
V455 - V460 Tau
See KK Tau.
V461 Tau See HZ Tau.
V462 Tau See SX Tau.
V463 - V465 Tau
See KK Tau.
V466 Tau See HZ Tau.
V467 - V469 Tau
See KK Tau.
V470 Tau See HZ Tau.
V471 Tau See EY Tau; mu alfa = + 0.117", mu delta = -0.020".
EA/D/(RS + WD) + XP. d = 0.0625P.
There occurs a
total eclipse of the white dwarf in Min I (A = 0.04m V,
0.36m U).
P var. Min I = 2440612.67083 + 0.52118321d*E
(JD2440570 - 970) [6250]; Min I = 2440898.80038 +
+ 0.52118376d*E (JD2440880 - 41360), Min I =
= 2441665.46153 + 0.52118329d*E (JD2441660 -
42100) [10058]; since JD2441900 -
see Table.
Wave-like distorsion with the amplitude from 0.05m
up to 0.27m and with the period close to the orbital
one is observed in the light curve outside eclipses;
sometimes there are also flares. The wave is migra-
ting on phase in the direction of phase decreasing
with a migration period of 191d [10060] or ~ 250d
[10061]. The period of white dwarf rotation derived
through X-ray observations Ppuls = 554.73s [10062].
V472 Tau See KK Tau.
V473 Tau P = 2.7800d?
V474 Tau See SX Tau.
V475 - V478 Tau
See KK Tau.
V479 Tau VB A (BC 8.90m, 59", 357deg); (k - b)2 = 0.40.
V480 Tau VB A (B 10.4m, 176", 303deg). See EY Tau.
V481 Tau See KK Tau.
V483 - V484 Tau
See EY Tau.
V485 Tau See KK Tau.
V486 Tau Epoch of Max (U) is given.
P =/ 10.61d? [10063].
V487 Tau See SX Tau.
On the photograph west is at the top and
south to the right.
V488 Tau See FL Tau.
V489 - V490 Tau
See KK Tau.
V491 - V492 Tau
See HZ Tau.
V493 Tau See KK Tau.
V494 Tau See SX Tau.
V495 - V496 Tau
See KK Tau.
V497 Tau See HZ Tau.
V498 Tau See SX Tau.
V499 Tau See KK Tau.
V500 Tau See FL Tau.
V501 Tau See SX Tau.
V502 Tau See FL Tau.
V503 Tau See SX Tau.
V504 Tau See KK Tau.
V506 Tau See SX Tau.
V507 - V516 Tau
See KK Tau.
V517 Tau See SX Tau.
V518 Tau VB B (A 14.4m; B 10", 80deg). See FL Tau.
V519 Tau See SX Tau.
V520 Tau See HZ Tau.
V521 Tau See SX Tau.
V522 Tau See KK Tau.
V523 Tau See SX Tau.
V524 Tau See KK Tau.
V525 Tau See SX Tau.
V526 Tau See KK Tau.
V527 Tau See SX Tau.
V528 Tau See KK Tau.
V529 - V530 Tau
See SX Tau.
V531 - V533 Tau
See KK Tau.
V534 - V536 Tau
See FL Tau.
V537 Tau See KK Tau.
V538 Tau See FL Tau.
V539 Tau See HZ Tau.
V540 - V541 Tau
See FL Tau.
V542 Tau See SX Tau.
V543 - V544 Tau
See KK Tau.
V545 Tau Max = 2444896.678 + 0.355d*E, M - m = 0.42P, A(V) =
= 0.09m [10052]. See FL Tau.
V546 Tau See SX Tau.
V547 Tau See KK Tau.
V548 Tau See HZ Tau.
V549 Tau See KK Tau.
V550 Tau See FL Tau.
V551 - V552 Tau
See KK Tau.
V553 Tau See SX Tau.
V554 Tau See KK Tau.
V555 Tau See SX Tau.
V556 Tau See KK Tau.
V557 Tau See SX Tau.
V558 Tau See KK Tau.
V559 - V560 Tau
See SX Tau.
V561 - V564 Tau
See KK Tau.
V565 - V566 Tau
See SX Tau.
V567 - V568 Tau
See KK Tau.
V569 Tau See SX Tau.
V570 - V577 Tau
See KK Tau.
V578 Tau See SX Tau.
V579 - V584 Tau
See KK Tau.
V585 Tau See IO Tau.
V589 Tau See IO Tau.
V594 - V595 Tau
See KK Tau.
V596 Tau See HZ Tau.
V597 - V601 Tau
See KK Tau.
V602 Tau See SX Tau.
V603 - V607 Tau
See KK Tau.
V608 Tau See SX Tau.
V609 Tau See KK Tau.
V610 Tau See FL Tau.
V611 - V612 Tau
See KK Tau.
V613 Tau See HZ Tau.
V614 Tau See KK Tau.
V615 Tau See SX Tau.
V617 - V622 Tau
See KK Tau.
V623 Tau See FL Tau.
V624 Tau The value
of P1(A1 = 0.01m) is given in the Table.
P2 = 0.017d, A2 = 0.007m. See FL Tau.
V625 - V626 Tau
See KK Tau.
V627 Tau See FL Tau.
V629 - V630 Tau
See KK Tau.
V631 - V632 Tau
See FL Tau.
V633 - V634 Tau
See SX Tau.
V635 Tau See FL Tau.
V636 Tau See SX Tau.
V637 Tau See KK Tau.
V638 Tau See FL Tau.
V639 - V640 Tau
See KK Tau.
V641 Tau Max = 2444896.744 + 1.22d*E; M - m = 0.5P, A(V) = 0.03m
[10052]. See FL Tau.
V642 - V644 Tau
See FL Tau.
V645 Tau See HZ Tau.
V646 Tau See FL Tau.
V647 Tau The value
of P1(A1 = 0.011m) is given in the Table.
P2 = 0.070d, A2 = 0.006m. See FL Tau.
V648 - V649 Tau
See KK Tau.
V650 Tau See FL Tau.
V651 Tau See KK Tau.
V652 Tau See FL Tau.
V653 Tau See SX Tau.
V654 Tau See HZ Tau.
V655 - V656 Tau
See KK Tau.
V657 Tau See SX Tau.
V658 - V659 Tau
See KK Tau.
V660 Tau Max = 2444896.453 + 0.23541d*E, M - m = 0.5P, A(V) =
= 0.20m [10052]. See FL Tau.
V661 - V663 Tau
See KK Tau.
V664 Tau See FL Tau.
V665 Tau See SX Tau.
V666 Tau See KK Tau.
V667 Tau See FL Tau.
V668 - V671 Tau
See KK Tau.
V672 Tau See SX Tau.
V673 Tau See HZ Tau.
V674 Tau See KK Tau.
V675 Tau See SX Tau.
V676 Tau See KK Tau.
V677 Tau See FL Tau.
V678 Tau See SX Tau.
V679 Tau See FL Tau.
V680 Tau See SX Tau.
V681 - V683 Tau
See KK Tau.
V684 - V685 Tau
See SX Tau.
V686 - V691 Tau
See KK Tau.
V692 Tau See HZ Tau.
V693 - V694 Tau
See KK Tau.
V696 - V697 Tau
See EY Tau.
V698 Tau Type INB?
V700 Tau See FL Tau.
V701 - V702 Tau
See KK Tau.
V703 Tau See FL Tau.
V705 - V707 Tau
See KK Tau.
V709 Tau See KK Tau.
V710 Tau VB A (B 16m, 3.5", 180deg).
V711 Tau VB A (B 8.83m, A = 8.023", E = 0.18, Porb = 2101 yr);
SB2 (Porb = 2.83774d [10070]).
Migration period of the distortion wave is about
10.5 yr [10072].
The range of combined light variation is given.
V712 - V717 Tau
See KK Tau.
V718 Tau See IO Tau.
V725 Tau SB1 (Porb = 110.8d [10076]).
X-ray outbursts occur periodically near
the periastron passages of the pulsar with P = Porb.
The amplitude of the corresponding variations of
visual brightness of the system A(V) = 0.03m. The pe-
riod of pulsar rotation Prot var [10077].
Prot = 104.17s (JD2442531), 103.806s (JD2442728),
103.882s (JD2443505), 103.8402s (JD2443620)
[10074]; 103.647s (JD2444521), 103.423s
(JD2445292), 103.3429ss(JD2445623) [10078].
V726 Tau Min II 11.2.
V727 Tau See KK Tau.
V728 Tau See SX Tau.
V729 Tau Max = 2439024.46 + 152.35d*E (JD2438680 - 39415);
Max = 2440127.78 + 313.86d*E (JD2439415 - 40510).
H2O maser.
V732 - V752 Tau
See KK Tau.
V753 Tau See SX Tau.
V754 - V757 Tau
See KK Tau.
V758 Tau See SX Tau.
V759 - V760 Tau
See KK Tau.
V761 - V762 Tau
See SX Tau.
V763 - V765 Tau
See KK Tau.
V767 - V772 Tau
See KK Tau.
V773 Tau THere are also quasisinusoidal light variations with
P = 3.43d and A(V) = 0.13m [10056].
V774 Tau VB A (B 6.96m, G5IV, 66.8", 315deg).
V775 Tau See EY Tau.
V776 Tau VB A (B 7.5m, 1.4", 333deg, 1958; C 8.7m, 77.2", 233deg,
1925); SB 1 (Porb = 57.25d). See EY Tau.
V777 Tau VB A (B 8.12m V, 0.0088", 173.2deg, 1980.6).
See EY Tau.
V778 Tau Min II 17.0. P var. Min I = 2438680.546 + 0.434842d*E
(JD2436528 - 38841); Min I = 2439765.488 +
+ 0.434846d*E (JD2439559 - 41031); since
JD2440129 - see Table.
V780 Tau VB A (B 15.8m V, 0.3", 310deg, 1974); mu = 0.364", P = 163deg.
V781 Tau Min II 9.3.
V782 - V784 Tau
See KK Tau.
V785 Tau See FL Tau.
V787 - V788 Tau
See KK Tau.
V789 - V790 Tau
See FL Tau.
V791 Tau See KK Tau.
V792 Tau Near V752
Tau. Identical to it?
See KK Tau.
V793 Tau See FL Tau.
V794 Tau See SX Tau.
V795 Tau See KK Tau.
V796 Tau See FL Tau.
V797 Tau See SX Tau.
V798 - V802 Tau
See KK Tau.
V804 Tau See KK Tau.
V805 Tau See EY Tau.
V807 Tau VB A (B = GH Tau, 21.4", 193deg).
V808 Tau Porb = 11.93d. See EY Tau.
alf Tau VB A (B 13.5m, M2V, 31", 110deg).
The star is surrounded by an infrared emission
envelope with the diameter of about 10".
See IO Tau.
zet Tau Min II 3.05.
tet 2 Tau
VB A (B 4.85m, 0.02077", 19.6deg, 1980.59); SB 1 (Porb =
= 140.728D, E = 0.75 [10087]).
The value of P1(A1 = 0.017m B) is
given in the Table. P1 var. Later P1 = 0.07541d (A1 =
= 0.023m B), P2 = 0.0831d (A2 = 0.013m B).
Possibly
eclipsing with the elements: Min = 2445358.38 +
+ 140.734d*E, A = 0.02m B.
See EY Tau.
lam Tau Min II 3.54. Triple system. The eclipsing sys-
tem rotates around the third component with P =
= 33.025d [10090].
See IO Tau.
ro Tau See EY Tau.
ips Tau VB A (B 6.5m, 0.020"). See EY Tau.
U Tel P var. Before JD2421000 Max = 2420992 +
+ 439.13d*E [0001]; since JD2423000 -
see Table.
RR Tel During 1889 - 1930 12m - 14m pg (according to [0625],
irregular variations; according to [0017], Max =
= 2411490 + 384d*E, with irregularities). During
1930 - 1944 12.5m - 16.5m pg, Max = 2430145 + 386.73d*E
[1649]; after 1938 an increase of mean brightness
And of the amplitude was noted. An outburst from
14m to 7m in October, 1944. In Max, 6.5m - 7.5m pg,
during JD2431500 - 33000; after JD2433100 began
to decline its mean brightness. Near the Max of the
outburst no periodic variations was noted. During
JD2441426 - 44899 5.06m - 6.74m J, P = 387d [9989],
M - m = 0.5P; Min (V) = 2442551 + 374.2d*E (1961 - 1981),
delta(V) = 0.25m for periodic changes [10029]; 9.8m - 10.7m B,
P = 395d (JD2443500 - 45500) [10030].
In the Max of the outburst the spectrum was CF5
without emissions. During the brightness decline a
rich emission spectrum was formed with lines of
hydrogen, forbidden lines of metals in high stages
of ionization, etc. Since the 1970-ies TiO absorption
bands are being noted.
Radio source, soft X-ray source.
RS Tel Semiregular variations,
P = 45.8d [8140]. IR excess.
RV Tel VB (0.6", 294deg, 1946). d = 0.02P.
SZ Tel Possibly
identical with the star alfa = 18h 13m 16s, delta = -53deg 39.2',
1950.0 (RR, 15m - 16.5m pg) [10032].
See TT Tel.
TT - TY Tel
In the region
of the globular cluster NGC 6584.
UY Tel VB.
AG Tel nf star of a pair.
AK Tel Very red.
AX Tel [A/H] = -0.7.
BL Tel The depth of Min II - 0.1m pg.
Semiregular variabi-
lity of pulsational character (7.09m - 7.26m V) is obser-
ved outside eclipses; sometimes it may be represen-
ted by P = 65.1d, but sometimes (1969) it cannot be
traced.
BO Tel [A/H] = -0.3.
CK Tel VB B (A 15.0m).
DZ Tel sf star of a pair.
FR Tel D >= 0.23P. Min II 14.0?
GH Tel P ~ 10.342d is possible.
GM Tel VB A.
GY Tel Min II 12.0.
HH Tel P var slightly.
HO Tel Min II 8.67.
HR Tel EW type
with twice longer P is possible.
IL Tel The ele-
ments need confirmation.
IQ Tel Min II 12.7.
KK Tel B - V: + 0.6m: (Min light).
KN Tel VB A (B 16m sf).
LW Tel Possibly identical to NSV
10695.
MT Tel mu alfa = -0.0127S, mu delta = -0.109".
[Fe/H] = -1.82. delta(S) = 9.9.
MV Tel See HR Tel.
MZ Tel See HR Tel.
NN Tel Min II 15.5.
NP Tel Min II 13.3.
NS Tel Min II 9.4.
NV Tel Min II 9.0.
OQ Tel sf star of a pair.
PR Tel Min II 11.35. Radio source
PKS 1925 - 524.
H beta fluctuates on ~ 5 min time scale.
PS Tel V39 (NGC 6584).
Probably non-member of the cluster.
P = 0.1422d or 0.1657d is possible.
PT Tel V27 (NGC 6584). Cluster non-
member.
PU Tel V24 (NGC 6584). Cluster non-
member.
PV Tel SB 2.
PX Tel V15 (NGC 6584). Cluster
non-member.
PZ Tel SB 2.
R Tri P var. Max = 2412167 + 267.3d*E (JD2412000 - 16000);
Max = 2416972 + 262.6d*E (JD2416000 - 20000);
Since JD2420000 - see Table.
Maser (H2O).
S Tri P var. Max = 2418541 + 248.9d*E (JD2418000 - 31000);
since JD2431000 - see Table.
T Tri P var. Max = 2420535 + 320.6d*E (JD2420000 - 27000);
since JD2427000 - see Table.
U Tri delta(S) = 1.3.
V Tri Min II 11.0.
X Tri VB A (B 13.3m, 6.7", 55.3deg, 1952).
Usual brightness in
Max 8.88. d = 0.013P; Min II 9.07.
According
to [10043], a two-peaked flare-like event of 35 min
duration (delta(V) = 0.33m) was observed at
JD2445594.4550.
P var. Min = 2422722.269 + 0.9715342d*E
(JD2422700 - 26600); Min = 2426946.508 +
+ 0.9715390d*E (JD2426600 - 33400); Min =
= 2433504.397 + 0.9715290d*E (JD2433400 - 35500);
Min = 2435687.422 + 0.9715352d*E (JD2435500 -
39200); Min = 2439375.373 + 0.9715277d*E
(JD2439200 - 42500) [7603]; since
JD2442500 - see Table.
Y Tri Var NO.2 (M33). VB A (B 17.28m B, 26.4" np).
RS Tri VB A (B 11.98m, 6.0", 214deg, 1962).
d = 0.016P; Min II 10.4, Min II - Min I = 0.56P.
RU Tri VB A (B 12m, 21.8", 88deg).
Min II 11.8:.
RW Tri The depth of Min I 1.12m - 2.21m.
D = 0.052P - 0.086P, d ~ 0.03P. P var? [3434, 9858,
9859].
Strong fluctuati-
ons of light outside eclipses. the lower the bright-
ness outside the eclipse, the deeper the Min. In J, K
light Min II of 0.16m J depth was found at the phase
0.50P [10053]. Flat spectrum of the accretion disc
with emission lines.
RX Tri Max = 2426577 + 192d*E (JD2426500 - 31800);
since JD2432800 - see Table.
According to [4029], P = 100d?
RY Tri Red.
ST Tri Min II 14.5.
SW Tri Blazhko effect is
possible.
SY Tri See SW Tri.
TT - TX Tri
In the region of the gala-
xy M 33.
TZ Tri ADS 1697 A (B 6.72m, F6V, SB2, Porb = 2.2365d,
3.9", 71deg, 1973); SB2 (P = 14.732d).
Secondary variations on ~ 100d time scale.
H and K CaII emission was noted only
for one of the two G - stars.
R TrA SB?
U TrA For
moments of Max0 (fundamental mode) see Table.
Max1 (first overtone) =
= 2443266.05 + 1.824881d*E.
RR TrA Min II 10.60, dII = 0.025P.
RW TrA (k - b)2 = 0.30. delta(S) = 1.
TW TrA VB.
AS TrA Min II 15.7.
BH TrA According to [4637], L type.
CI TrA Possibly P < 0.3d.
DV TrA Three Max and three Min are observed during a cycle.
Max1 (fi = 0.0P) 13.2m; Max2 (fi = 0.2P) 14.2m; Max3
(fi = 0.6P) 13.5m. Min1, Min2, Min3 ~ 16.0m.
EH TrA Shallow Min II is
possible.
EK TrA n star of a pair.
For the mean cycle between normal ma-
xima see Table. the mean cycle between supermaxi-
ma 442.1d (JD2435200 - 39700), 551.5d (JD2439700 -
44050). Superhumps (delta(M) = 0.26m V) with P = 0.06492d,
M - m = 0.26P [9945].
EL TrA Min II 10.9.
EM TrA Min II 10.4.
EN TrA According to [7934],
RV: type.
EP TrA Min II 9.5.
EQ TrA MIN II 9.0.
P var. Min = 2416267.614 + 2.709220d*E (JD2416000 -
29000); since JD2429000 - see
Table.
ER TrA P > 220d.
FH TrA The ele-
ments need confirmation.
FK TrA See FH TrA.
FM TrA P >= 220d.
GN TrA Min II 12.0.
HP TrA Deep Min II.
The elements
need improvement.
HV TrA Min II? 14.8. Min II - Min I = 0.55P.
IM TrA P >= 150d. Epoch of Min is given.
IW TrA Min II 14.5:. See FH TrA.
KX TrA 2U 1639-62? P.K.326 -10deg 1.
Gas velocities up to 5000 km/s
[9958].
KY TrA TrA X-1 = A1524-61.
KZ TrA 4U 1626-67. Lx/Lopt ~ 2000. VB B (A 14.9m; B25",
189deg).
Barycentric
period parameters for pulses [4534]: Min =
= JED 2443931.2394789; P = 7.6776762s, DP/dt =
= (-4.95 +-0.02)*10**-11. delta(m) pulse = 0.02m - 0.17m.
Porb = 2491.06s or 2492.32s [4558].
Flares with delta(m) up to 0.4m with intervals ~ 20 min
correlated with X-ray flares [4536].
LP TrA VB A (B 11.5m, 25", 123deg; C 12.0m, BC 6").
T Tuc P var. Max = 2410138 + 250.76d*E (JD2410000 -
14400); Max = 2414900 + 248.88d*E (JD2414400 -
22000); Max = 2432160 + 250.00d*E (JD2422900 -
35000); since JD2437700 - see
Table.
U Tuc See UW Tuc.
P var. Max = 2421190 + 258.12d*E (JD2412600 -
22000); Max = 2427487 + 262.83d*E (JD2422000 -
28000); Max = 2437808 + 257.70d*E (JD2428000 -
39150); since JD2440900 - see
Table.
V Tuc See UW Tuc.
The depth of Min II 0.11m.
W Tuc (k - b)2 = 0.09, delta(S) = 7:. P var?
Z Tuc In the
region of the Small Magellanic Cloud.
RR Tuc See Z Tuc.
VB A (B 17m, 6", 90deg).
RS - RU Tuc
See Z Tuc.
RV Tuc See Z Tuc. VB.
RW - RZ Tuc
See Z Tuc.
SS Tuc See Z Tuc. HV 1877.
Earlier was erroneously identi-
fded with HV 1887.
ST Tuc See Z Tuc.
SU Tuc See Z Tuc. HV 1922.
According to [9980], alternatively may be
identical to HV 1920.
SV - SW Tuc See Z Tuc.
SX Tuc See Z Tuc. VB (B 16m? P).
SY Tuc See Z Tuc. Min II 15.4.
SZ Tuc See Z Tuc.
TT Tuc See Z Tuc. VB A (B 17m, 8" sp).
TU Tuc See Z Tuc.
TV Tuc See Z Tuc.
The variable's position in 2' to the north
of CPD -73deg 64 [9980] makes it impossible to identify
it with HV 2041.
TW - TX Tuc
See Z Tuc.
TZ Tuc See UW Tuc.
VB A (B 13m sp).
UW Tuc In the region of the Small Magellanic Cloud.
SMC non-member.
UX Tuc See UW Tuc. In the neighbourhood OF 47
Tuc; probably cluster non-member.
P var. [Fe/H] = -1.8.
VV - VW Tuc
See Z Tuc.
VZ Tuc See Z Tuc.
XZ Tuc See Z Tuc.
YY Tuc The elements need
improvement; current elements with the epoch from
[7984] are given.
(k - b)2 = 0.03. delta(S) = 8:.
AD Tuc See UW Tuc. delta(S) = 4.9.
AF Tuc See UW Tuc.
AH Tuc See UW Tuc. P var.
AI Tuc See UW Tuc.
In the region of the globular cluster NGC 362. P var.
AK Tuc See UW Tuc. P var.
AL Tuc See UW Tuc.
AM Tuc The elements
should be checked.
[Fe/H] = -1.82. delta(S) = 9.9.
AO Tuc The elements
need improvement.
delta(S) = 5.
AP Tuc See UW Tuc.
AQ Tuc See UW Tuc.
In the region of the globular cluster 47 Tuc.
Min II 10.48.
AR Tuc See UW Tuc.
AS - AT Tuc
See Z Tuc.
AU - AV Tuc
See UW Tuc.
AW - AY Tuc
See Z Tuc.
BC Tuc See Z Tuc.
BD Tuc See UW Tuc.
BE Tuc See Z Tuc.
BF Tuc See Z Tuc. [A/H] = -0.7.
BG Tuc See UW Tuc.
BH Tuc See Z Tuc. VB A (B 14.28m, 10" n).
BS Tuc (k - b)2 = 0.10.
BT - BZ Tuc
See Z Tuc.
CF Tuc See UW Tuc. Soft X-ray source. Distortion
wave. delta(m) = 0.057m [10065]. Min II 7.52.
tet Tuc For
the period of the main oscillation (A = 0.0132m) see
Table. Other instable frequences were also noted.
R UMa Maser (H2O).
S UMa S 1.5/6 e. P var. Max = 2398325 + 224.51d*E
(JD2394000 - 2405000); Max = 2405290 + 230.20d*E
(JD2405000 - 10500); Max = 2417530 + 223.96d*E
(JD2410500 - 23500); Max = 2426324 + 228.53d*E
(JD2423500 - 28800); since JD2428800 -
See Table.
T UMa Maser (H2O).
W UMa ADS 7494 A (B 12.35m, 6.5", 44deg, 1963).
dI = 0.037P; Min II 8.43, dII = 0.028P.
Soft X-ray source.
LX/Lbol = 1.7*10**-4.
P var. Min I = 2420980.8093 + 0.333638880d*E
(JD2416000 - 21000); Min I = 2420980.8093 +
+ 0.333636993d*E (JD2421000 - 33000) [1760];
Min I = 2435918.4169 + 0.33363832d*E (JD2433000 -
41000) [5327]; since JD2441000 -
See Table. The light curve shape, including depths of
minima, var. A moving wave with delta(m) = 0.025m y and
P ~ 1100d [10067] was noted. A flare (delta(m) = 1.5m,
lambda 3300 A, delta(lambda) = 50 A, JD2438511.7, delta(t) = 7 min) was
announced [5788]. The system contains gaseous
streams, dark spots on the surface of the components.
H and K CaII emission.
Z UMa Usually 2 Max and
2 Min during a cycle.
RV UMa P var. Max = 2417861.434 + 0.4680618d*E
(JD2417800 - 25000); Max = 2425053.675 +
+ 0.4680654d*E (JD2425000 - 29000) [0188];
Max = 2438459.945 + 0.468062d*E (JD2429000 -
40000) [3506]; since JD2440000 -
See Table.
Blazhko effect, Pi = 92.12d
(JD2436229 - 38114) [9835]. Pi var.
[Fe/H] = -1.04; delta(S) = 3.5.
RW UMa DI < 0.08P; Min II 10.34, DII = 0.10P.
[Fe/H]A = -0.1, [Fe/H]B = -1.0. P var?
Distortion wave, A = 0.11m V.
SS UMa In the galaxy NGC 5457 (M 101).
SU UMa The cycle of normal
maxima 5d - 35d [9782, 3791].
Three different mean values of
the mean cycle of supermaxima change each otHer
being active at different time intervals: P1 = 161.5d;
P2 = 203.9d; P3 = 248.1d (
= 201.7d) [9276].
Porb = 2.06d/N (N = 26, 27, 28) or 3.1h.
Surrounded by a faint
halo (28' diameter) of soft X-ray sources.
SW UMa SB.
Superior conjunction of the accretion disc T =
= 2445376.8601 + 0.0567433d*E [9836].
SX UMa P var strongly. Before JD2418800
Max = 2416200.486 + 0.3071148d*E; Max =
= 2418800.213 + 0.3071345d:*E (JD2418800 - 22500)
[0001]; Max = 2422653.5032 + 0.30711855d*E
(JD2422500 - 26000) [10083]; Max = 2426400.418 +
+ 0.3071555d*E (JD2426000 - 29500); Max =
= 2430000.250 + 0.3071301d*E (JD2429500 - 34000),
Max = 2438508.751 + 0.3071363d*E (JD2434000 -
39000); since JD2441500 - see
Table.
[Fe/H] = -1.82, delta(S) = 9.9.
SZ UMa mu alfa = -0.4853s, mu delta = + 0.148".
TU UMa P var [3506]. [Fe/H] = -1.05, delta(S) = 7.6.
TW UMa d = 0.002P; Min II 12.3:.
TX UMa Min II 7.13. P var. Min I = 2416426.801 + 3.063297d*E
(JD2416000 - 22000); Min I = 2427926.492 +
+ 3.063337d*E (JD2424200 - 30000); Min I =
= 2433440.431 + 3.063300d*E (JD2430000 - 38000)
[9839]; since JD2438000 - see
Table.
TY UMa P var, non-linear term:
+ 6.4d*10**-11*E**2.
dI = 0.05P, dII = 0.00P.
The light curve shape var.
12.10 <= Min I <= 12.14, 12.06 <= Min II <= 12.12.
UX UMa The shape of the eclipse light curve, the
mean level of light outside eclipses, the depth of
Min var. Deviations from the tabulated elements may
reach +-0.002d. Rapid brightness oscillations
(28.54s <= P <= 30.02s) are sometimes observed [7304].
Soft X-ray source.
UY UMa Min II 12.9.
VV UMa Min II 10.26. P var. Min I = 2439245.408 + 0.6873793d*E
(JD2425600 - 40200) [9843]; Min I = 2440768.6280 +
+ 0.687367d*E (JD2440200 - 42700); since
JD2442700 - see Table.
VX UMa Maser (H2O).
WX UMa Mu alfa = -0.4094s, mu delta = +0.955", VB B (A = BD +44deg 2051,
dM2, 8.74m V; B 28", 133deg; common mu). Soft
X-ray source. LX/LV = 0.095.
XY UMa Mu alfa = -0.0055s, mu delta = -0.175".
P var.
Non-linear term: +2.77d*10**-11*E**2.
The brightness outside eclipses var by
0.16m V. The depth of Min I is 0.48m - 0.67m, that of
Min II is 0.19m. Migrating wave.
XZ UMa Min II 10.2. P var? Min = 2444986.445 + 1.2223105d*E
(JD2414990 - 45000); since JD2445000 -
see Table.
AA UMa Min II 11.53, Max II 10.94.
The elements should
be checked.
AC UMa VB B (A = BD + 65G671, 9.97m V, B-V = +0.50m; B 19",
114deg, 1957).
The chart in [8953] is
wrong.
AD UMa Blazhko effect is
possible. Pi = 35d - 40d, delta(A) = 0.2m.
AE UMa The fundamen-
tal mode P0 is given in the Table.
P1 = 0.066527d, Pbeat = 0.293616d [9869].
Max 10.86 - 11.10, Min 11.46 - 11.52.
AF UMa d = 0.05P.
AK UMa The elements need
improvement.
AN UMa The epoch of Min for periodic (P =
= Porb) light variations with A <= 1m B is given. Min II
is present. B - V = 0.0 in Max light, +0.5 during an
eclipse; U - B = -1.1. Circular polarization in B light
-9% to -35%; linear polarization 0% - 13% with a
sharp Max near Max light. Rapid changes (A = 0.03m,
f = 0.4 - 0.8 Hz). The mean light level and the light
curve shape var. During the low state (B ~ 19m) the
light variability with porb disappears, emission li-
nes occur only during 10% of Porb, IR excess is no-
ted. Soft X-ray source, var. Emissions of H, HeI,
He II, NIII, FeII.
AW UMa dI = 0.06P:; Min II 7.08, dII = 0.11P.
The light curve shape var.
P var. Min I = 2442150.4385 + 0.43873234d*E
(JD2438000 - 42200); since JD2442200 -
see Table.
AX UMa P var. Max = 2435951.354 + 0.53510d*E (JD2435900 -
38200) [4375]; during JD2445000 -
45900 - see Table.
BE UMa d = 0.006P. Outside eclipses var
14.8m <= B <= 16.0m (reflection effect). The depth of ec-
lipses for lambda lambda 3330 - 3700 A is greater than 4.3m,that
for lambda lambda 5265 - 6005 A is 1.5m.
BG UMa Min II 10.93.
Alternative type EW.
BH UMa Min II 12.3.
BI UMa Min II 15.8.
BK UMa [Fe/H] = -1.29, delta(S) = 6.6.
BL UMa Min II 16.2.
BM UMa The depth of Min II 0.80m.
BN UMa [Fe/H] = -1.65, delta(S) = 8.9.
BP UMa D <= 0.04P.
The elements need confirmation.
CE UMa In the region of the
cluster of galaxies Abell 1213. SN 1966 omikron?
CF UMa Groombridge 1830 B (A = BD +38deg 2285, V = 6.45m,
B - V = +0.75m, G8 subdwarf, mu alfa = + 0.339s,
mu delta = -5.81"; B 2", 165deg).
A possible flare on February 27, 1968. A brightening
of the combined light by 0.6m pg on April 27, 1939
[9881]. Maybe the object does not exist [9882].
CH UMa X-ray source 1E 1003 + 67.
LX/Lopt = 0.04.
CM UMa P var?
CQ UMa The epoch of Max in U and B light
coinciding with that of Min in V light is given.
A(U) = 0.06m, A(B) = 0.06m.
CR UMa The elements for
Max in U light are given. In B and V bands no perio-
dicity is apparent.
A(U) = 0.03m.
CW UMa Mu = 0.27", P = 300deg.
DF UMa ADS 8242A (B 11.4m, 1.8", 60deg, 1960).
The data for combined brightness are given
in the Table.
SB 1, Porb = 1.033824d.
Mu alfa = +0.0131s, mu delta = -0.038".
Besides rapid va-
riations ( = 10.14m, delta(V) = 0.05m), long term varia-
tions are possible.
DG UMa Blazhko effect is
possible.
DK UMa Soft X-ray source,
lg Lx/Lv = -3.5. [Fe/H] = -0.38.
DL UMa Eclipses with P = 0.42d [4706].
DM UMa SB 1 (Porb = 7.492d).
Min = 2444026.97 + 7.478d*E (1979 - 1982); 1981 -
1984 - see Table.
Two Min in the light curve in
1981 - 1982.
DN UMa ADS 8347 ABC (A 7.2m vis; B 9.0m vis, 0.121", 142.0deg,
1981.5; C 8.3m vis, 4.0", 42deg, 1980; D = BS 4561,
A1pCrEuSr:, V = 7.03m, B - V = +0.01m, 63.0", 114deg).
The range of combined brightness for the three com-
ponents is given. It is not known which of the compo-
nents varies. The component D was used as a com-
parison star.
Min II 6.73, Min II - Min I = 0.504P.
eps UMa SB (P=4.15A).
Interferometric
binary? (0.053", 94.5deg, 1975.4).
In 1976 - 1983 attempts to re-
solve the binary interferometrically were not success-
ful.
In the UMa moving
cluster; mu alfa = +0.0131s, mu delta = -0.010".
ips UMa ADS 7534 A (B 11.5m, 11.3", 295deg, common mu).
mu alfa = -0.0382s, mu delta = -0.156".
The light cur-
ve shape and A var.
R UMi H2O maser.
S UMi P var. Max = 2422604 + 321.9d*E (JD2413000 -
23000); Max = 2432200 + 331.5d*E (JD2423000 -
32800); Max = 2436080 + 322.5d*E (JD2433000 -
37000); Max = 2439011 + 326.5d*E (JD2437000 -
41500); since JD2441500 - see
Table.
T UMi P var. Max = 2428332 + 315.48d*E (JD2416500 -
29500); Max = 2436415 + 310.05d*E (JD2429500 -
37200); Max = 2442389 + 315.5d*E (JD2437200 -
43600); since JD2443600 - see
Table.
U UMi P var. Max = 2416975 + 323.1d*E (JD2416500 -
21000); Max = 2428804 + 331.3d*E (JD2421000 -
29780) [0001]; Max = 2429789 + 320.6d*E (JD
2429780 - 34600) [0960]; Max = 2434600 + 331d*E
(JD2434600 - 36300); Max = 2437853 + 322.6d*E
(JD2436300 - 39000); since JD2439000 -
see Table.
V UMi Mean brightness var with P2 =
= 760d.
W UMi Min II 8.66; d = 0.02P. P var?
Non-linear term in the elements
is possible: -7.7d*10**-10*E**2.
X UMi P var? Max = 2424224 + 343d*E (JD2423800 - 25100)
[0684]; since JD2438100 - see
Table.
RR UMi SB (Porb = 749.4d [9896]).
RT UMi Min II 10.86.
RU UMi Min II 10.20.
RZ UMi Min II 13.5.
alf UMi VB A (B 8.20m, F3V, 18.3", 218deg); SB 1 (Porb = 10969d,
E = 0.655 [9904]). P var.
There is a non-linear term in the elements:
+1.9877d*10**-7*E**2.
The amplitude of light and
radial velocity variation decreased in 1982.
A(V) = 0.04m (1984).
gam UMi P var. Max = 2424301.78 + 0.14335d*E [10097]; Max =
=2427904.468 + 0.14335d*E [10098].
Elements given in the Table represent ob-
servations in 1964 - 1968. According to [9906] Vr var
in 1922 with P = 0.108449d.
eps UMi VB A (B 12.5m, 76.9", 3deg). Min II 4.21.
S Vel Min II 7.83; d = 0.041P. P var? There
is a non-linear term in the elements given in the
Table: +4.47d*10**-9*E**2.
W Vel P var. Max = 2415053 + 384.3d*E (JD2414600 - 17400);
Max = 2426080 + 399.9d*E (JD2422400 - 27300);
Max = 2429990 + 388.0d*E (JD2427300 - 30100);
Max = 2438328 + 398.7d*E (JD2430100 - 38800);
since JD2438800 - see Table.
OH emission.
Y Vel P var. Max = 2415900 + 438.6d*E (JD2411500 -
15900); Max = 2419930 + 447.7d*E (JD2415900 -
19930); Max = 2425755 + 452.8d*E (JD2421600 -
27600); Max = 2434150 + 439.5d*E (JD2427600 -
34200); since JD2434200 - see
Table.
Z Vel P var. Max = 2415445 + 435.96d*E (JD2415000 -
25100); Max = 2425462 + 417.99d*E (JD2425100 -
29700) [0960]; since JD2429200 -
See Table.
RR Vel Min II 10.9.
RS Vel P var. Max = 2410403 + 421d*E (JD2410400 - 16800)
[9961]; since JD2415450 - see
Table.
RU Vel VB A (B 12m sf). According to [0017],
Max = 2414390 + 63d*E.
RW Vel P var. Max = 2413553 + 430.4d*E (JD2413500 -
18500); Max = 2420610 + 465.7d*E (JD2418500 -
25700); since JD2425700 - see
Table.
RX Vel Min II 10.5.
RY Vel [A/H] = -0.3. P var. Max = 2440246.67 + 28.1270d*E
(JD2419000 - 40250) [5366]; since
JD2443900 - see Table.
SW Vel P var. Max = 2434872.95 + 23.473d*E-3.75d*10**-5*E**2
(JD2412500 - 35500) [9636]. Since
JD2440700 - see Table.
SX Vel The light curve has double maximum. The epoch of
The primary (second) maximum is given in the Table.
TT Vel Min II 10.7.
UW Vel In the region of
the open cluster NGC 3033.
YZ Vel Min II 12.8; DII = 0.040P; Min II - Min I = 0.537P.
ZZ Vel Min II 10.0.
AA Vel Min II 10.3.
AC Vel Min II 9.11.
AF Vel (k - b)2 = 0.06. Blazhko
effect is possible [10110].
AH Vel SB? [10111]. See AK Vel.
AI Vel Mu = 0.11", P = 76deg; (k - b)2 = 0.23.
Light oscillations with the period
P0 given in the Table are superimposed by oscilla-
tions with P1 = 0.08620868d and twice smaller amplitu-
de. According to [10112] P0 is constant, P1 is increa-
sing.
AK Vel In the region of
the open cluster Collinder 173.
AL Vel d = 0.072P.
AO Vel See AK Vel.
Min II 9.55:.
There is apsidal line motion.
There is a sinusoidal term
In the elements given in the Table: +0.058d sin fi,
wHere fi = 2pi(E - 5338)/11500, and E values are
counted from JD2415810.66.
Min II = 2424270.125 + 1.5845993d (E - 5338) -
- 0.058d sin fi; Min II - Min I = 0.792d - 0.116d sin fi.
AP Vel P1 = 2.19984d; P1/P0 = 0.703. M - m var (0.25P <= M - m <=
<= 0.50P) [3710].
AQ Vel d = 0.05P. The depth of Min II 0.05m.
AS Vel Min II 8.4; Min II - Min I = 0.55P.
AT Vel d = 0.03P. See AK Vel.
AU - AW Vel
See AK Vel.
AX Vel The first overtone mode light variation elements with the
period P1 are given in the Table; the amplitude of
the first overtone mode light variation A1 exceeds
that of the fundamental mode, A0:A1(V) = 1.5A0(V).
For the fundamental mode P0 Max hel = 2443878.885 +
+ 3.673174d*E.
P1/P0 = 0.706; M - m var: 0.24P <= M - m <= 0.50P:.
AY Vel Min II 9.7.
AZ Vel Min II 13.0. See AK Vel.
BB Vel P < 20d. See AK Vel.
BC Vel Min II 12.3.
BD Vel d = 0.04P.
BE Vel Min II 12.5.
BF Vel The depth of Min II 0.04m.
BM Vel Min II 13.0. In
the region of the open cluster NGC 2547.
See also AK Vel.
BO Vel Min II 14.2.
BP Vel Min II 13.7.
BR Vel The shape of
the light curve varies.
BT Vel Min II 14.8.
BU Vel Min II 10.96; Min II - Min I = 0.522P. See AK Vel.
BV Vel See AK Vel.
BW Vel Min II 14.3.
BX Vel In the region of
the open cluster Tr 10.
BZ Vel Min II 10.4; Min II - Min I = 0.57P.
CK Vel D ~ 0.3d.
CL Vel Min II 13.4.
CR Vel d = 0.05P.
CS Vel [A/H] = 0.1.
Possible member of the open cluster Ruprecht 79.
CU Vel The period of superhumps ~ 0.08d,
A = 0.4m [10115].
CV Vel Min II 7.17.
CW Vel d = 0.024P. The depth of Min II 0.1m pg.
CZ Vel Min II 11.1.
DF Vel Min II 13.4.
DH Vel Min II 13.7.
DK Vel VB A (B 12.50m, 22", 315deg; C 16m, 10", 60deg).
DL Vel Min II 12.1.
DM Vel P = 123d?
DQ Vel Min II 11.0.
DS Vel Min II 10.8.
DT Vel (k - b)2 = 0.24.
DX Vel Min II 10.3.
In the region of the open cluster Col 213.
EH Vel Min II 13.4.
EL Vel See AK Vel.
EO Vel Min II 11.90, DII = 0.07P.
Apsidal motion: Min II - Min I = 3.15d + 0.00003d*E.
Min II = 2441716.75 + 5.32969d*E.
EP Vel In the region
of the open cluster IC 2395.
ES Vel Min II 12.7.
ET Vel Min II 12.1.
EU Vel Min II 13.8.
EY Vel d = 0.04P:.
FM Vel Min II 12.9.
FS Vel delta(S) = 10.
FT Vel Min II 10.5.
FW Vel Min II 10.0.
FX Vel Min II 10.5. See BR Vel.
FY Vel Min II 7.03. Type ELL? [6827].
FZ Vel VB A (B 12.08m, 24.2", 338deg).
GG Vel VB A (B 11.2m, 6", delta(alfa) = 0). P = 2.950432d?
GP Vel 6.90. Min II - Min I = 0.55P.
See BR Vel.
There are probably long-period light
oscillations: Min = 2442681.6 + 93.3d*E (A ~ 0.02m)
[10051].
The period
of X-ray pulses var: 282.8913s (1975.5) [10125];
282.919s (1975.7) [10126]; 282.869s (1976.4),
282.838s (1976.9) [10127]; 282.80s (1978.9) [10128];
282.745s (1979.3), 282.7874s (1980.3), 282.87s (1981.0)
[10129]; 282.93s (1981.9 - 1982.9); 282.9306s (1983.2)
[10078].
GV Vel In the region of
the open cluster NGC 2660.
HU Vel Pulsar PSR 0833-45.
In the nebula Vela SNR.
Star M [8276].
The pulsed
radiation varies in radio, optical and gamma rays
with P = 0.089s.
P var [10136 - 10139]: P = 0.089233318274s
(JD2442553 - 680), P = 0.089234713929s (JD
2442700 - 848), P = 0.089244007685s (JD2443654 -
676), P = 0.089245406487s (JD2443719 - 850) [10137];
P = 0.089256985348s (JD2444795.84) [10138].
HV Vel A member of the open
cluster IC 2391.
HW Vel P = 0.26133d? See HV Vel.
HX Vel VB A (B 7.1m, 0.3", 313deg, 1949); See EP Vel.
Min II 5.50:.
HY Vel VB A (B 5.7m, 76.6"); see HV Vel.
Min II 4.90.
IL Vel A var (0.02m <= A <= 0.15m). Beat period
10.075d (Min A = 2443175.5 + 10.075d*E).
IM Vel VB A (B 9.73m, 3.3", 179deg, 1948).
The double wave of light variations
with rotation period Prot = 2.85204d and A = 0.03m is
superimposed by oscillations with the periods
P1 = 0.00812815d (A1 = 0.0043m), P2 = 0.00808206d
(A2 = 0.0035m), P3 = 0.00810503d (A3 = 0.0008m), P4 =
= 0.004052519d (A4 = 0.0009m), P5 = 0.004064065d
(A5 = 0.0004m), P6 = 0.004041031d (A6 = 0.0004m),
P7 = 0.00815128d (A7 = 0.0004m) [9208].
IN Vel P = 65 - 70d,
IP Vel VB A (B 11.2m V, 2.1", 200deg, 1929). P > 1.25d.
IQ Vel Min II 12.94; Min II - Min I = 0.500P.
IS Vel A(U) var: 0.005m <= A(U) <= 0.018m.
IT Vel Min II 7.08. P = 23.52d?
gam 2 Vel
VB A (B 4.22m, 41.3", 220deg).
SB2 (Porb = 78.5002d [10119]). In
HII region.
T0 = 2433633.0
is the epoch of the conjunction where the
O component is in front [10119].
lam Vel VB A (B 14.8m, 18.2", 137deg).
omi Vel See HV Vel. P(VR) = 2.74d. P = 2.76d? SB1?
The epoch
of the light maximum is given. Close binary system?
R Vir P var. Max = 2381914 + 145.77d*E (JD2338900 -
2402000); Max = 2402321 + 144.90d*E (JD2402000 -
18000); Max = 2418268 + 145.48d*E (JD2418000 -
30000); Max = 2430489 + 148.32d*E (JD2430000 -
34000); Max = 2434193 + 144.63d*E (JD2434000 -
38500); Max = 2438829 + 147.45d*E (JD2438500 -
43000); since JD2443000 see
Table.
Maser (SiO).
S Vir P var. Max = 2399014 + 374.7d*E (JD2398600 -
2405000); Max = 2412970 + 376.2d*E (JD2412000 -
23500, on average); Max = 2423502 +
+ 381.52d*E (JD2423500 - 23000); since
JD2433000 see Table.
Maser (H2O, SiO).
T Vir Maser (OH, H2O, SiO).
V Vir P var. Before JD2427000 Max = 2400467 +
+ 250.17d*E; Max = 2427225 + 246.54d*E (JD2427000 -
31500); since JD2431500 - see
Table.
W Vir The epoch of Min is given. P var.
Min = 2404151.168 + 17.2707d*E (JD2403000 - 23200);
Min = 2423200.837 + 17.2634d*E (JD2423200 - 29700);
since JD2429700 see Table.
The light curve
shape var.
[Fe/H] = -1.03.
X Vir VB A (B 12m, dK4, 0.6', ~ 50deg).
The brightenings
of 1871 and 1882 may be due to misidentification
[1651].
Z Vir mu alfa = +0.0098S, mu delta = -0.120".
P var. Max = 2409683 + 309.19d*E (JD2408000 -
18500); since JD2418500 see
Table.
RS Vir Maser (OH, H2O, SiO).
P var. Max =2412592 + 351.29d*E (JD2412000 -
31000); since JD2431000 see
Table.
RT Vir Maser (OH, H2O, SiO).
According
to [10145], observations of 1970-1977 are not in ag-
reement with the P value in the Table.
RU Vir P var? Max = 2425120 + 435.9d*E (JD2414000 -
31500); since JD2431500 see
Table.
RV Vir P var. Max = 2412272 + 268.39d*E (JD2412000 -
31500); since JD2431500 see
Table.
RX Vir VB (B 13.0m vis, 1.1", 107deg, 1939).
According to
Photoelectric observations [6450, 8837], 8.72m - 8.81m V.
Const? [6450].
SS Vir P var. Max = 2415910 + 352.75d*E (JD2415900 -
21500); Max = 2421913 + 361.7d*E (JD2421500 -
26500); Max = 2428359 + 350.12d*E (JD2426500 -
40000); since JD2440000 see
Table.
ST Vir P var. Max = 2425005533 + 0.4108494d*E (JD2422000 -
29100) [10146]; Max = 2436702.513 + 0.4108168d*E
(JD2433000 - 39000) [3415]; since
JD2439000 see Table.
Blazhko effect?
delta(S) = 0.8.
SU Vir P var. Max = 2415040 + 213.7d*E (JD2415000 - 19500);
Max = 2419926 + 210.96d*E (JD2415000 - 31500);
Max = 2437378 + 210.2d*E (JD2431500 - 38500);
since JD2438500 see Table.
SV Vir P var? The mean elements
are given.
Maser (H2O).
SZ Vir Possibly EW
with a very small A.
TV Vir VB A (B P).
TW Vir Porb = 0.182666d [9430].
Variability of ellipsoidal character in H
light: P = Porb/2, A(H) = 0.13m.
X-ray source.
TX Vir VB A (B 15m, 0.3' P).
TY Vir [Fe/H] = -1.7.
TZ Vir P2 = 6900d is superimposed?
UU Vir [Fe/H] = -0.3. delta[S] = 0.7.
UW Vir d = 0.011P.
P var. Min = 2419942.513 + 1.8106818d*E (JD
2415000 - 34500); since JD2441000
see Table
UY Vir d = 0.014P; Min II 8.1.
VV Vir Min II 12.2:.
VW Vir SN 1895 (NGC 4424).
XX Vir [Fe/H] = -1.5. delta(S) = 9:.
YZ Vir [A/H] = -0.9.
AD Vir P var. Max = 2425259.259 + 0.5522109d*E
(JD2419000 - 31000); since JD2431000 -
see Table.
AF Vir P var. Max = 2429051.697 + 0.4838214d*E
(JD2419500 - 36000); Max = 2436718.3758 +
+ 0.4838386d*E (JD2436000 - 37500) [10159];
since JD2440000 see Table. DM var.
AG Vir The depth of Min II up to 0.44m.
The light cur-
ve shape and a Var.
dI = 0.03P:, dII = 0.66P. Min II - Min I = 0.512P.
P var. Min = 2434487.4297 + 0.6426489d*E (JD
2424500 - 34500); since JD2434500
see Table.
AH Vir mu alfa = +0.0015S, mu delta = -0.111"
ADS 8472 A (B 13.2m, 1.3", 17deg).
The combined brightness is given,
dI = 0.07P. The depth of Min II 0.53m, dII =
= 0.00P.
The light curve
shape var.
P var. Min = 2434841.3963 + 0.40751843d*E
(JD2425000 - 35000) [5222]; Min = 2435573.710 +
+ 0.40752192d*E (JD2435000 - 41400); Min =
= 2441411.460 + 0.40753186d*E (JD2441400 - 44000);
since JD2444000 see Table.
AK Vir VB B (A = BD -17deg 3996; B 44", 286deg).
AL Vir P var [A/H] = -0.7.
AN Vir P2 ~ 1000d is superimposed.
AO Vir VB A (B 11.4m vis, 6.9", 321deg, 1956, common
Vr). delta(M) is
possibly in error because of the companion.
P var. Max = 2413949 + 256.88d*E (JD2412900 -
21000); since JD2421000 see
Table.
AS Vir P var. The Table gives the mean elements
valid after JD2425600. Blazhko
effect? [3506].
(k - b)2 = 0.08.
AT Vir P var. Max = 2426831.367 + 0.5258053d*E (JD
2420500 - 35000) [0188]; since JD2435000 -
see Table.
(k - b)2 = 0.00, delta(S) = 6.0.
AU Vir [Fe/H] = -1.84, delta(S) = 10.1.
AV Vir delta(S) = 5.5.
AW Vir Min II 11.67.
AX Vir Min II 10.24.
AY Vir Maser (H2O).
AZ Vir Min II 11.37.
BB Vir Blazhko effect?
BC Vir P var. Max = 2419922.289 + 0.56451468d*E
(JD2419900 - 30100);
The Table gives current elements.
BD Vir P var. Min = 2424971.720 + 2.548410d*E
(JD2424900 - 32000); since JD2432000 -
see Table.
BF Vir Min II 10.72. Total eclipses.
P var. Min = 2416595.67 + 0.64057d:*E (JD2414000 -
19000); Min = 2440331.809 + 0.64057631d*E
(JD2426000 - 41000); since JD2441000 -
see Table.
BH Vir Min II 10.24. Distortion wave?
(delta(V) = 0.04m).
BN Vir P var. Max = 2419865.422 + 0.39127585d*E
(JD2419800 - 28300); since JD2432600 -
see Table.
BO Vir P var. Max = 2419513.388 + 0.52005916d*E
(JD2419500 - 33000); since JD2433000 -
see Table.
BQ Vir P var?
BS Vir [Fe/H] = -1.84. delta(S) = 10.1.
BV Vir P var. Max = 2426070.488 + 0.4965803d*E
(JD2419900 - 28500); since JD2436600 -
see Table.
BW Vir P var. Max = 2420247.403 + 0.4706660d*E
(JD2420200 - 26800); since JD2426800 -
see Table.
CG Vir Min II 10.9.
CK Vir [Fe/H] = -2.0.
CM Vir d = 0.05P. P var. Min = 2425411.330 + 3.40167d*E
(JD2423900 - 28400) [0001]; during
JD2432200 - 34200 see Table.
CS Vir The epoch of Max in B
light is given.
SB (Porb = 1618d).
IR excess (4.8 mkm).
CU Vir ADS 9152 A (B 11.9m, G1V, 60", 212deg).
CW Vir The epoch of min is given.
CX Vir The depth of Min II 0.30m.
DK Vir According to [10189], P1 = 0.1162d, P2 =
= 0.1086d. (k - b)2 = 0.20.
DL Vir SB (Porb = 2286d).
The spectrum shows the A-component of the eclipsing
system and the G8III star around which the eclipsing
system is orbiting.
DM Vir Min II 9.49. DII = DI.
DN Vir P >= 100d.
DT Vir Mu alfa = -0.044s, mu delta = -0.02". SB?
Rotation period 1.535d [10014], A = 0.05m V.
DV Vir Blazhko effect?
EF Vir According to [4784], const?, 16.1m pg.
EP Vir IR excess (4.8 mkm).
EQ Vir SB; [Fe/H] = -0.08; mu alfa = -0.018s, mu delta = -0.09".
Min = 2441129.585 + 3.914169D*E + 0.0001803345d*E**2,
A = 0.10m V, M - m = 0.40P.
Soft X-ray source,
lg FX/FV = -2.07.
EW - EY Vir
P >= 100d.
FF Vir The P value for
magnetic field variations is given.
FG Vir ADS 8471 A (B 13.51m, 25", 352deg, 1909;
C 11.85m, 74", 195deg, 1909).
FI Vir Mu alfa = +0.043s, mu delta = -1.22".
FL Vir VB AB (A = 0.76", P = 16A).
Both components show flares? The range
of combined brightness is given.
Mu alfa = -0.118s, mu delta = +0.26".
FM Vir SB2, Porb = 38.324d.
FN Vir Mu alfa = -0.064s, mu delta = +0.28". SB?
X-ray source, LX/Lbol = -3.55.
FO Vir Min II 6.67.
FQ Vir Deep Min II.
GG Vir Multiperiodicity,
0.023d <= P <= 0.083d, A <= 0.02m.
GH Vir P var.
GK Vir The secondary is a red dwarf (M0 - M6).
GL Vir Mu alfa = -0.087s; mu delta = + 0.23".
GM Vir P ~ 1.6d/n.
GQ Vir Mu alfa = -0.045s, mu delta = -0.44".
GR Vir The depth of Min II 0.41m.
GU Vir P var. Max = 2439236.36 + 0.466562d*E
(JD2438100 - 39300); during
JD2441300 - 42600 see Table.
alf Vir The Table gives the epoch of
Min for the ellipsoidal variability and Porb.
The depth of Min II up to
0.08m. SB 2. e = 0.205 +- 0.004.
Apsidal motion: Pi = 108a +- 5a.
Pulsations: P var, P = 0.17378587d
(1908 - 1956); since 1956 Max = 2445405.63 +
+ 0.17378680d*E [10181]. A var.
3 companions according to lunar occultation obser-
vations: 3.1m, 0.0025"; 4.5m, 0.05"; 7.5m, 0.5".
Soft X-ray source,
LX/Lbol = 2.9*10**-8.
psi Vir Binary? (lunar occultations).
R Vol P var. Max = 2415238 + 441d*E (JD2394100 -
2418800) [10143]; since JD2422700
see Table.
S Vol P var. Max = 2415042 + 397.6d*E (JD2415000 - 24200),
Max = 2428880 + 392.1d*E (JD2423000 - 28900),
Max = 2434113 + 401.7d*E (JD2428900 - 34900),
Max = 2434910 + 387.2d*E (JD2434900 - 39200);
since JD2439200 see Table.
T Vol P var. Max = 2413135 + 189.8d*E (JD2413100 - 14600);
Max = 2416870 + 171.8d*E (JD2414600 - 16900);
Max = 2416870 + 176.8d*E (JD2416800 - 24400);
Max = 2424460 + 170.8d*E (JD2424400 - 27200);
Max = 2429925 + 182.3d*E (JD2427200 - 30000);
since JD2440000 see Table.
RX Vol P < 20d?
ST Vol SP component of
a very close pair.
SV Vol The shape of the
light curve varies.
TX Vol Min II 10.5. P var. Min I = 2416789.869 + 5.38845d*E
(JD2415100 - 26000), Min I = 2431150.345 +
+ 5.3887d*E (JD2426000 - 31400), Min I =
= 2433542.609 + 5.388d*E (JD2431400 - 33600)
[0001]; since JD2433600 see
Table.
R Vul P var. Max = 2400169 + 138.3d*E (JD2400100 - 02700),
Max = 2402779 + 136.76d*E (JD2402700 - 19800),
Max = 2419880 + 137.45d*E (JD2419800 - 24400),
Max = 2424413 + 136.76d*E (JD2424400 - 28500
[0960]; Max = 2429331 + 135.9d*E (JD2428500 - 32000)
[0001]; since JD2432000 see
Table.
S Vul In the region of
the open cluster C 1947 + 272 [10123].
P var. Max = 2401772 + 67.37d*E (JD2401760 - 6400),
Max = 2408180 + 67.70d*E (JD2408170 - 14950),
Max = 2415285 + 68.26d*E (JD2415300 - 22800),
Max = 2423468 + 67.72d*E (JD2423450 - 27200),
Max = 2428227 + 68.18d*E (JD2428220 - 31300)
[0761]; Max = 2432775 + 67.51d*E (JD2431300 -
34500) [10148]; Max = 2437150 + 68.66d*E
(JD2436800 - 39600), Max = 2441507 + 67.344d*E
(JD2439600 - 43000) [10124]; since JD
2443000 see Table.
[A/H] = 0.1.
T Vul P var. Max = 2419372.151 + 4.435589d*E (JD2409880 -
34000); since JD2434000 see
Table.
V Vul Min II 8.65. P var. Min I = 2414912.9 + 74.96d*E
(JD2414900 - 20840), Min I = 2420909.8 + 75.686d*E
(JD2420900 - 24810), Min I = 2425072.9 + 76.344d*E
(JD2425050 - 30000), Min I = 2430023.5 + 75.957d*E
(JD2430000 - 32500) [10149].
Study of period variation
and changes of Min II by Min I see also in [0767,
10150].
W Vul In the region of
the open clusters NGC 6882, NGC 6885.
X Vul P var. Max = 2420636.337 + 6.319301d*E (JD2417000 -
34000) [0768]; since JD2435000 -
See Table.
Z Vul VB A (B 12.0m, 13", 359deg). Min II 7.58. P var. Min I =
= 2425456.117 + 2.454926d*E (JD2413200 - 37000)
[0063]; since JD2437000 - see
Table.
RS Vul Min II 6.86; Min II - Min I = 0.508P.
RU Vul A var. P var. Max = 2416266 + 155.95d*E
(JD2415000 - 36000), Max = 2436779 + 150.7d*E
(JD2436000 - 38800), Max = 2438855 + 153.4d*E
(JD2438800 - 41620), Max = 2441193 + 138.5d*E
(JD2441620 - 42600); since JD2442600 -
see Table.
RX Vul P var. Max = 2420301 + 438d*E (JD2418900 - 22500)
[4018]; since JD2424700 - see
Table.
RZ Vul Slow variations
of mean brightness with P = 1410D and A = 2m are su-
perimposed by fluctuations with the cycle 40 - 100d
and A up to 1m.
SU Vul See W Vul.
SV Vul [Fe/H] = 0.23. P var.
THere is a nonli-
near term in the elements given in the Table:
-0.0001814d*E**2.
SX Vul In the region of
the open cluster NGC 6940.
UU Vul The co-ordinates are wrong?
[10156].
VV Vul Min II 12.1; d = 0.026P. P var. Min I = 2416670.527 +
+ 3.411224d*E (JD2416600 - 27500) [0134];
since JD2426000 - see Table.
VW Vul Porb = 0.0731d [10160].
VY Vul Min II 14.4:.
WW Vul There is quasi-periodicity in light minima with the cycle
404d.
XZ Vul Min II 11.4. P var. Min I = 2426477.525 + 3.0895116d*E
(JD2416900 - 36000) [4427]; since
JD2436000 - see Table.
AB Vul The depth of Min II 0.02m.
AD Vul Min II 0.010P.
AF Vul Min = 2436545.23 + 0.954d*E (JD2436200 - 900) [3148].
AR Vul In the region of
the open cluster Stock 1.
AT Vul Min II 9.3; d = 0.02P.
AW Vul MIN II 10.9; d = 0.020P.
AX Vul d = 0.018P.
AY Vul d = 0.020P. P var. Min hel = 2436128.388 + 2.4124239d*E
(JD2418500 - 40700); since JD2440700 -
see Table.
AZ Vul Min II 11.9.
BB Vul In the region of
the open cluster NGC 6940.
BE Vul VB A (BC 11.92m, 50", 320deg). Min II 9.90. P var.
Min I = 2426144.490 + 1.55205d*E
(JD2426140 - 28880), Min I = 2430698.203 +
+ 1.5520442d*E (JD2430690 - 34660), Min I =
= 2435340.373 + 1.552052d*E (JD2435340 - 40070);
since JD2440100 - see Table.
BF Vul Elements given in the Table
represent well only the bright maxima. The fainter
maxima are represented by the elements: Max =
= 2427731 + 95.4d*E.
BI Vul Min II 14.86. P var? Min I = 2424759.70 + 0.251828d*E
[0193]; since JD2444750 - see
Table.
BN Vul delta(S) = 7. P var. Max = 2414815.759 + 0.5941295d*E
(JD2414000 - 30000) [0388]; Max = 2434244.333 +
+ 0.59412538d*E (JD2430000 - 36000) [0616];
Max = 2438265.386 + 0.59412763d*E (JD2436000 -
41000) [9009]; since JD2441000 -
see Table.
BO Vul Min II 10.6. P var. Min I = 2429984.332 + 1.9459123d*E
(JD2415000 - 30000) [0007]; Min I = 2432379.766 +
+ 1.9459206d*E (JD2427000 - 35000), since
JD2435300 - see Table.
BP Vul Min II 10.5.
BS Vul Min II 11.10.
BT Vul d = 0.03P; Min II 12.3.
BU Vul P var. Min = 2431006.204 + 0.5689904d*E
(JD2426500 - 31100) [0001]; since
JD2433500 - see Table.
BV Vul S 6.5/6-.
BW Vul P var. Max = 2424000.171 + 0.20102229d*E
(JD2424000 - 26500), Max = 2426500.079 +
+ 0.20102933d*E (JD2426500 - 31500), Max =
= 2432000.054 + 0.20103513d*E (JD2431500 - 41000);
since JD2441000 - see Table.
CD Vul Min II 11.9.
CK Vul Max 2331186:. Connected
with nebulae.
Type NR?
CS Vul Min II 13.6.
DR Vul Min II 9.19; DII = 0.132P.
THere is apsidal motion with the period 37.8 years.
Elements given in the Table contain supplementary
terms: -0.07165d*sin (0.05863deg*E) - 0.00269d*
*sin (0.11726deg*E).
Min II = 2440301.7934 + 2.2508645d*E + 0.07165d*
*sin (0.05863deg*E) - 0.00269d sin (0.11726deg*E).
P var? [10185]. The
depth of minima varies.
DY Vul VB A (B 13.0m V, 14", 300deg).
EH Vul P var. Max = 2429609 + 185d*E (JD2429600 - 30600);
since JD2430800 - see Table.
EP Vul S 6.5/5.
EQ Vul Min II 12.5; Min II - Min I = 0.31P; DII = 0.050P, dII =
= 0.010P.
ER Vul P var. Min I = 2440182.2593 + 0.69809510d*E
(JD2433100 - 40200) [8592]; since JD
2440100 - see Table.
7.35m <= Min II <= 7.44m.
The shape of the light
curve and depths of minima vary.
ES Vul VB A (B 10.1m, 1.6", 126deg).
ET Vul [A/H] = -0.4. P var. Max = 2425110.63 + 54.33d*E
(JD2422900 - 26600), Max = 2432875.80 + 54.33132d*E
(JD2432700 - 35430), Max = 2438656.99 + 53.81d*E
(JD2436050 - 39035), Max = 2439253.55 + 54.24d*E
(JD2439035 - 40990) [10168]; since
JD2441900 - see Table.
EU Vul Min II 13.3.
EV Vul Min II 11.9. P var. Min I = 2428750.459 + 2.822084d*E
(JD2428400 - 36400) [4027]; Min I = 2436748.37 +
+ 2.82220d*E (JD2436380 - 750) [3732]; since
JD2441500 - see Table.
EX Vul d = 0.03P.
EY Vul The depth of Min II 0.05m.
FG Vul See BB Vul.
Star 120.
The epoch of light minimum
is given.
FH Vul P var. The elements given in the
Table are valid since JD2436000.
FK Vul Blazhko effect.
FM Vul Min II 13.0.
FN Vul d = 0.02P; Min II 14.2.
FP Vul Min II 15.6.
FQ Vul Min II 12.9.
Apsidal motion with P = 280 years. Correction of mispints
in [4248] see in [4244].
FR Vul Probably the
period must be doubled.
FS Vul Min II 15.2.
FU Vul sp component of a clo-
se pair.
FW Vul Min II 12.9.
FY Vul See FU Vul.
Cycle 30 - 70d [4027].
FZ Vul Min II 13.9.
GG Vul P var. Max = 2427681.0 + 106.5d*E (JD2427500 -
28850); since JD2428850 - see
Table.
GH Vul P = 2.5d?
GI Vul Min II 13.8.
GK Vul Red.
GN Vul Min II 12.4; d = 0.04P.
GO Vul Min II - Min I = 0.515P. The depth of
Min II 0.03m.
GP Vul Min II 11.2; Min II - Min I = 0.48P.
GQ Vul nf component of a close triple group of stars.
P var. Max = 2434399.825 + 12.647241d*E (JD
2426100 - 38000) [4414]; since JD2444600 -
see Table.
GR Vul Min II 13.3.
GT Vul Min II 15.8.
GU Vul Min II 12.2.
GV Vul See FR Vul.
HI Vul Min II 12.6.
HP Vul The depth of Min II 0.04m.
HS Vul Min II 14.2.
HU Vul Blazhko effect?
HV Vul P var. Max = 2437165.449 + 0.419906d*E (JD2437100 -
38670); since JD2438670 - see
Table.
See HU Vul.
HW Vul P var. Max = 2429077.0 + 75.44d*E (JD2427190 -
29080), Max = 2429077.0 + 73.94d*E (JD2429070 -
32470); since JD2432350 - see
Table.
IU Vul P var. Max = 2434656 + 320.2d*E (JD2432700 -
37860) [4427]; since JD2437860 -
See Table.
IW Vul Min II 13.1.
KN Vul Min II 13.4.
KO Vul Red.
KS Vul Very red.
LT Vul Multiperiodicity:
P1 = 0.109414d, A1(V) = 0.0234m; P2 = 0.11094d,
A2(V) = 0.0074m; P3 = 0.1215d, A3(V) = 0.0070m
(JD2444054 - 096) [10173];
P1 = 0.109621d, A1(B) = 0.0340m; P2 = 0.093528d,
A2(B) = 0.0136m (JD2444071 - 465) [10193].
LU Vul Nova Vul 1968 N2.
LV Vul Nova Vul 1968 N1. VB A (B 18m, 6", 115deg).
LW Vul Min II 16.3.
MN Vul Min II 16.1; Min II - Min I = 0.518P; DII = 0.10P.
MO Vul Min II 14.8. P var?
MR Vul P2 = 111.0d?
MT Vul Multiperiodicity:
P2 = 119.93d (A2 = 0.3m), P3 = 25.02d (A3 = 0.4m:).
MX Vul P = 181.8d?
NO Vul Min II 14.1.
NS Vul VB A (B 8.8m, A0, 0.73", 273deg, 1978.6),
The range of
combined light variation is given.
PS Vul VB A (B 10.0m, 0.4", 105deg, 1980.0); SB 2.
PT Vul P1 = 256.12714s (A1 = 1.14%), Max1 =
= 2445166.660914 HJED; P2 = 256.33205s (A2 = 1.09%),
Max2 = 2445166.659424 HJED; P3 = 128.11496s (A3 =
=0.37%), Max3 = 2445166.660024 HJED.
mu = 0.1508", P=1.6deg.
PU Vul Pre-outburst SP M4 (1958). Gradual
light increase in 1977 - 79 up to 8.7m V; in 1979 A =
= 0.29M V, Min I = 2443943.39 + 78.12d*E [10197]. In
the max of 1979 Sp F5Ia - F8-9I. In February 1980
an abrupt light decrease started; the star reached
V = 13.65m by early September. By September, 1981
the star recovered from the deep Min of 500d duration.
During the 1980 - 81 minimum Sp M5 with TiO bands,
emissions of H alfa, NaD, [OII], FeII, rare earths. In
1982 - 84 8.35m - 8.87m V, Sp became F again. Simeti-
mes H alfa, H beta emissions have been detected, often
with P Cyg profiles.