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 - Mi