R And S5/4.5e.
S And SN (NGC 224).
W And S7.5/1-e.
X And S5/7-e.
Z And The light curve is characterized
Z And by outbursts up to 4m with intervals of 10 - 20
Z And years. In the intervals cyclic variations are observed with
Z And the mean period of 632d and variations with cycles of
Z And several days and Delta(m) ~ 0.1m - 0.5m. The spectrum is
Z And symbiotic, with features of a late M giant, narrow
Z And low-excitation emission lines (Bleq) and forbidden lines
Z And characteristic of highly excited nebulae.
RR And S6/3.5e.
RT And Min II 8.88; DI = DII = 0.17P; dI = dII = 0.00. P var.
RT And Nonlinear term: -6.33*10**(-11)*E**2. During
RT And JD2433477 - 43878 linear elements are satisfactory:
RT And Min = 2441141.8888 + 0.62892984d*E. Period changes
RT And according to a sine law are possible [8002].
RU And P var. Max = 2419857 + 243.0d*E (JD2412800 -
RU And 20000); Max = 2434551 + 233.24d*E (JD2420000 -
RU And 34550). Since JD2435000 - see Table. Delta(m) ~ 4m - 5m
RU And (before JD2429600), ~1m (JD2429600 ~ 33600), up to 3m
RU And (JD ~2436000), ~1.5m (JD ~2436700). In 1970 - 1972
RU And showed quite irregular variations.
RW Aur VB A (B 12.5m, dM0e, 1", 2, 254deg). The companion probably flares
RW Aur with an amplitude 0.5m - 0.7m [3197, 3198] Possible period of
RW Aur axial rotation is 100d [7067] OH emission
RX And SB (P = 0.21173d). Cyclic variations with P ~ 38s - 54s
RX And were observed after a normal maximum; after a short
RX And maximum no periodicity was found [8004].
SS And Two long period variations are also observed:
SS And P = 650d, P = 3800d.
ST And P var. Max = 2418370 + 337.3d*E (JD2418000 - 28000).
ST And Since JD2428000 - see Table.
SU And VB A (B 12.77m V, F0V:, 15").
SV And The magnitude in Max varies periodically, P = 930d,
SV And P = 5400d? [2146].
SW And [Fe/H] = +0.16. P var. Nonlinear term:
SW And -1.229d*10**(-10)*E**2 [1959]. Since 1959
SW And Max = 2436466.828 + 0.442270121d*E [6929].
SW And The shape of the light curve varies with
SW And Pi ~36.83d = 83.28 P. The deviations (O - C) satisfy
SW And the elements of Blazhko effect
SW And Max(O - C) = 2436816.23 + 36.921d*N. Secular trend
SW And and cyclic (P ~2a) variations of (O - C) are possible
SW And [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 +
TW And 4.122739d*E (JD2420050 - 32000). Since JD2432000 - see
TW And Table.
TZ And P1 = 118d: [0882].
TZ And Mean magnitude varies with P2 = 974d [0098]. P = 135d
TZ And (JD2437545 - 38377) [3367].
UU And P var. Min = 2428832.536 + 1.486311d*E (JD2421455 - 23740)
UU And [2262]; Min = 2428832.465 + 1.48629d*E (JD2428830 - 35012)
UU And [0745]. Since JD2441100 - see Table.
UW And P var. Before JD2430000 Max = 2418585 + 236.7d*E. Since
UW And JD2436000 - see Table.
WW And d = 0.012P.
WX And P var. Max = 2422613.614 + 3.0012544d*E (JD2422610 - 34712)
WX And [1240]. The Table gives current elements. d = 0.03P
WX And in 1972 and probably varies.
WZ And Min II 11.9. P var [2262]. Min = 2435075.342 + 0.695662d*E
WZ And (before JD2440500); probably
WZ And Min = 2440872.290 + 0.6956576d*E since JD2440500.
WZ And The elements in the Table represent all the observations
WZ And satisfactorily.
XX And P var. Max = 2418001.938 + 0.7227486d*E (1908 - 1932);
XX And Max = 2427106.403 + 0.7227591d*E (1932 - 1946) [2264].
XX And Since 1946 - see Table. Delta(S) = 9. Blazhko effect:
XX And 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,
XZ And 8593]. Min = 2432883.6046 + 1.3572708d*E (JD2431700 -
XZ And 36150) [1977]; Min = 2441954.340 + 1.357293d*E
XZ And (since JD2436200). The elements in the Table represent all
XZ And the observations satisfactorily.
AA And Min II 10.5.
AB And Min II 10.20. P var. Period increased suddenly in 1953
AB And ( ~JD2434500); no period changes later [2509, 5222].
AB And Elements since 1953 - see Table.
AC And Unusual multiperiodical variable. Second oscillation:
AC And Max = 2432467.373 + 0.71124243d*E; P3 = 0.421069d [8187],
AC And see also [8294, 8295]. Delta(S) = -1:.
AD And Min II 11.6. Depth of minima in yellow light: 0.62m (Min I),
AD And 0.58m (Min II) [3141]. Min II - Min I = 0.494P. P var.
AD And Min = 2428718.402 + 0.9861940d*E (JD2417460 - 29640)
AD And [1983]. Since JD2428700 - see Table.
AE And In the M31 galaxy. Strong UV continuum.
AE And Emissions: H, He I, Fe II, [Fe II].
AF And In the M31 galaxy. Strong UV continuum.
AF And Emissions: H, He I, Fe II, [Fe II].
AG And According to [8296], DSCT:, Min = 2442636.5868 + 0.0347d*E,
AG And A = 0.5m.
AM And VB A (B 0.25' S).
AN And Min II 6.09. The existence of the third body in
AN And 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
AT And on period variations and a detailed study.
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 +
BL And 0.7223779d*E (JD2415800 - 33900) [1995]. Since JD2433900 -
BL And see Table.
BX And ADS 1671 A (B 9.7m, 20", 59deg). Min II 9.15. Possible
BX And period change from 0.61011222d to 0.61011534d (~1952).
BX And 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
CC And light curve shape vary with a period 5.23714d or 10.469d
CC And [8016]. According to [3120], 4 periods are present:
CC And P2 = 0.0632083d. First overtone was not found. Other
CC And periods are resonances.
CG And P var: 3.7430d (1950), 3.7394d (1963) [5224].
CG And Cyclic period changes are possible.
CG And According to [6941], short period oscillations (P = 2h 04m)
CG And are present. A number of observers do not find short-term
CG And variability.
CM And According to [0821], Max = 2428380 + 140d*E and Max =
CM And 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
DR And [2275]; then P changed abruptly. Delta(m) changes by ~0.3m,
DR And Max A1 = 2436078.8 + 69.486d*N1, Max A2 = 2437646.65 +
DR And 69.719d*N2. Other possible cycles are 2000d (interaction
DR And 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
DZ And [6945], since 1961 is in Max light all the time. According
DZ And to [6946], the spectrum is not characteristic of RCB stars.
DZ And According to [8660], the star was bright near the moments
DZ And of Min light given in [4008].
EG And P = 40d or 80d [8020].
EG And Absorption spectrum with overlaying emissions of high
EG And excitation [4434, 8598]. Strong variable magnetic field
EG And [4435]. Long period variations of light are observed.
EG And Radial velocities profiles and equivalent widths of lines
EG And vary with P = 470d [8596] (SB? [8597]). Possibly is
EG And analogous 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.
ET And The Table gives the epoch of Max light. Observations may
ET And be represented by the periods 0.723d and 1.61553d
ET And [8022, 7946]. According to [8023], in June - December 1977
ET And Min = 2443337.4725 + 0.49925d*E, other periods are
ET And not satisfied by observations. According to [8599],
ET And Max(U) = 2439751.28 + 0.617135d*E (1967 - 1971).
ET And SB, Max(Vr) = JD2443718.0 + 48.304d*E [8301].
ET And Photometric periods could not be found in radial
ET And velocities.
EX And Possible Min II 13.0:, Min II - Min I = 0.55P.
EY And I - K = 5.38;
EY And the presence of a dust envelope is possible [6947].
FF And 10.35m - 10.42m V outside flares; M - m = 0.50P.
FF And Porb = 2.170304d [8024]. According to photometric
FF And observations, P = 2.14d (1971), P = 2.15d (1972),
FF And 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).
GN And Different authors give spectral types F0 III, F2V, Am
GN And (probably based on different criteria).
GP And Delta(m) changes with P2 = 0.64d.
GP And A wave with P3 = 0.012161d is present. The mean
GP And magnitude and the shape of the light curve vary
GP And [8302].
GQ And ADS 246 B (A = GX And; B 37", 61deg). B - V = +1.80.
GQ And X-ray source.
GR And Min (magnet.field) = 2442288 + 525d*E.
GR And Magnetic field varies (-250 to -1030 Gauss). Period of
GR And changes of C1 is near 1.5 years [7893]. According to [6257],
GR And 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?
GX And (conflicting data).
GY And SB1 (P = 273.2d [7324], P = 272.99d [8303]).
GY And For spectral changes, variations of light and magnetic
GY And field it is possible that P = 23a [7004] or 20.60a [8303].
GY And [8022] gives P ~36.5d and Delta(V) ~0.049m. Periods 4.92a
GY And and 1.8d may exist [8303].
GZ And B - V: +0.77, +0.82. ADS 1693 A (B 11.13m, 8", 31deg).
GZ And Min II 11.58. P var?
GZ And The period is based only on Minima I [6830] and
GZ 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
HN And (P = 106.27d [7435]).
HQ And According to [8659], a probable cataclysmic binary;
HQ And 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 According to [8659], a probable cataclysmic binary;
HV And similarity to AM Her and AN UMa is noted.
HY And In the region of M 31.
HZ And In the region of M 31. P > 100d. Red.
IL And d = 0.02P.
IM And In the region of M 31.8.
IO And According to [8659], a probable cataclysmic binary;
IO And similarity to AM Her and AN UMa is noted.
IP And d = 0.02P:.
KK And The light curve has double-wave shape
KK And [7740]. Long period variations were found [7955].
KU And I - K = 4.63.
KU And SR type is possible. Surrounded with a dust envelope [8029].
KX And SB2 (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.
V0369 And VB (0".1, 128 deg, 1986.9).
V0374 And Not identical with BD+44 422.
alf And SB (P = 96.6960d). VB A (B 11.2m, 80").
alf And Epoch of Max U light is given.
alf And Hbeta index varies in the range of ~0.02m with P
alf And ~3h [8030]. Rapid rotation.
zet And Depth of Min II 0.1m. SB.
zet And Unstable light curve. Most notable
zet And variations on the rising branch of Max II [8030].
zet And Many peculiarities in the spectrum.
lam And SB1 (P = 20.52d).
omi And v sin i = 300 km/s; VB(0.3"; possibly
omi And also 0.05" - according to speckle-interferometric data).
omi And Shell spectrum appeared and disappeared several
omi And times since 1890. Different authors attributed
omi And the star to EB type. According to [5955], The changes
omi And of light may be explained also by intrinsic
omi And variations of a single shell star. They are represented
omi And by elements: Min I = 2439470.628 + 1.0185d*E.
omi And According to [2572], Min I = 2436174.430 +
omi And 1.5998398d*E. The periodogram analysis shows
omi And a stable peak at P ~0.84d [8032]. A possible shell
omi And 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 -
T Ant 34688), P = 5.8976d (JD2434688 - 37660) [5387].
T Ant The Table gives mean elements which satisfy all
T Ant observations well enough.
V Ant OH, H2O maser.
Z Ant Mean brightness varies with P = 1143d.
SW Ant Min II 14.6.
UZ Ant P var?
WY Ant P var. P = 0.57430871d (JD2414000 - 22070); P =
WY Ant 0.57431618d (JD2422070 - 25600); P = 0.57431216d
WY Ant (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
RT Aps the light curve [6152].
TY Aps Delta(S) = 3.
YY Aps The period is probably 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 Epoch of Min is given.
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
KZ Aps changes with superimposed variations of eclipsing
KZ Aps 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 (delta2 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,
R Aqr OII. Variable radio source. SiO maser. The secondary may
R Aqr be an accreting white dwarf. The star is embedded in an
R Aqr expanding gaseous nebula several hundred years
R Aqr old. A cycle ~24a and longer-term variations are
R Aqr possible in the changes of radial velocities and period.
U Aqr Strong bands of 12C2, CN,
U Aqr lines of SrII, YII in the spectrum; hydrogen deficiency.
U Aqr 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
RY Aqr JD2428000); Min = 2440824.410 + 1.966620d*E
RY Aqr (JD2428000 - 41000); Min = 2440824.410 +
RY Aqr 1.966611d*E (JD2441000 - 43800). Since
RY Aqr JD2443800 P = 1.966554d?
RY Aqr The Table gives elements representing
RY Aqr observations after JD2428000 with the accuracy +-0.1d.
ST Aqr Min II 9.37. P var. Min = 2423640.271 + 0.78101367d*E
ST Aqr (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
VY Aqr (1962), ~9m pg [3129].
WX Aqr Blazhko effect is possible.
XZ Aqr P var. Before JD2437913 P = 2.059187d.
YZ Aqr B - V = 0.49 (in Min). (k - b)2 = 0.06.
YZ Aqr Small fluctuations of period are possible.
AE Aqr Unusual flare X-ray system with pulsar. Becomes bluer
AE Aqr in Max. In Min B - V = +0.92. Shows rapid irregular
AE Aqr variations, which differ it from UV stars and UG
AE Aqr system, though the spectra are somewhat similar.
AE Aqr Simultaneous photoelectric and spectroscopic observations
AE Aqr [3131] show the existence of two types of flares:
AE Aqr 1) intensification of emission lines accompanied by
AE Aqr brightening in U and B; 2) intensification of continuum
AE Aqr leading to brightening in U, B and V ("white flare").
AE Aqr Detailed spectroscopic investigation [1971].
AE Aqr Porb = 0.41165794d + 1.12*10**(-10)*E, The epoch
AE Aqr T0 = JD2439030.621 [8672]. In the X-ray band
AE Aqr (0.1 - 4.0 keV) pulsations with P = 33.0767s are observed
AE Aqr [8673]. In the optical range pulsations with
AE Aqr P0 = 33.076737s as well as with P1 = 16.5s were noted
AE Aqr [8674, 8675].
AT Aqr Min II 14.7.
AX Aqr P var. Before ~JD2427367 Max = 2425417.60 + 0.388135d*E
AX Aqr [3113].
AY Aqr Min II 14.3.
BH Aqr P var. Before ~JD2431150 Max = 2426948.411 + 0.5258022d*E
BH Aqr [3113].
BI Aqr Min II 13.1.
BK Aqr Close companion.
BL Aqr Waves from 80 to 125d. Mean magnitude changes
BL Aqr 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 =
BN Aqr 2426577.901 + 0.46963401d*E [3113].
BN Aqr According to [5391] Max = 2429395.742 +
BN Aqr 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
BV Aqr light in Max up to 0.75A.
BW Aqr d = 0.01P. Min II 10.8. Min II - Min I = 0.484P.
BW Aqr Jensch [0189] considers the secondary Min to be the
BW Aqr main one.
BX Aqr d = 0.027P.
CD Aqr d = 0.012P. Min II 10.2.
CE Aqr According to [2548], no
CE Aqr variations were found in visual observations during
CE Aqr several months in 1954 - 1958. According to [3138],
CE Aqr 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
CY Aqr Max = 2434308.4314 + 0.061038509d*E. The shape of
CY Aqr the light curve probably varies. For M - m different
CY Aqr authors give values from 0.23p to 0.40p. Beat phenomenon
CY Aqr 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
DV Aqr with Delta(m) ~0.1m and P < 3h, presumably of DSCT
DV Aqr type nature. Some sources give A3 for the spectral
DV Aqr type. Shell spectrum was observed in May, 1975.
DV Aqr Spectral lines were filled with emission and therefore
DV Aqr weak, strong absorption in H and K CaII lines was present.
DV Aqr Shell effects were not present in the spectra taken in
DV Aqr 1971 - 1973 [8062].
DX Aqr VB B (A 7.0m, K0III; B 3.7", 244deg). SB1. d ~0.015P.
DX Aqr Depth of Min II ~0.3m.
DX Aqr 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.
EM Aqr Period and amplitude vary on very short time
EM Aqr scale. Light and colour vary approximately in phase.
EM Aqr 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. SB1. The unique eclipsing system of a red
FF Aqr star and probably a blue hot subdwarf. The amplitude of
FF Aqr the eclipse is 0.15V, 0.4B, 1.2U. The magnitude in Max
FF Aqr varies by 0.35V, 0.33B, 0.22U. Variable shape of light
FF Aqr curve. Strong emissions H and K CaII, Halpha in the
FF Aqr 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).
FK Aqr mu alpha = +0.455", mu delta = -0.067". SB2 (P = 4.08322d
FK Aqr [0313]). Flares Delta(U) = 0.7 [0344].
FL Aqr BDS 11854 B (A = FK Aqr; B 24", 352deg, 1966).
KV Aqr One deep fading overlapping a brightening trend.
omi Aqr Shell or disk spectrum is observed.
pi Aqr The brightness increased by ~0.2m V
pi Aqr in 1957 - 1975, the star became redder. Balmer
pi Aqr continuum in emission. Rapid changes in emission
pi Aqr lines and in polarization. Existence of a disk
pi Aqr or a shell is possible.
R Aql P var. Max = 2440038 + 297d*E (JD2427850 - 40000).
R Aql Since JD2440000 - see Table.
R Aql For the whole observed period
R Aql Max = 2399190 + 346.932d*n - 0.239303d*n**2;
R Aql Pn = 348.980d - 0.554202d*n + 0.000552309d*n**2 [3143].
R Aql H2O, OH and SiO maser. Radiobursts.
U Aql B - V: +0.84, +1.24. P var. ADS 12503 A (B 14.00m,
U Aql 35", 349deg, 1900; one more companion 11.7m V, 2", 230deg,
U Aql 1934).
W Aql S 6/6e. Composite spectrum near Min light; a companion
W Aql (F5 - F8) may exist [3502].
Y Aql Depth of Min II 0.03m. SB1.
RR Aql Maser H2O, OH, SiO.
RT Aql Maser H20, OH, SiO.
SY Aql Maser H2O, OH.
SZ Aql B - V: +1.04, +1.82. P var [2392]. Before JD2420260
SZ Aql P = 17.1359d. Current elements - see Table.
TT Aql B - V: +0.96, +1.62. P var. [2392]. Before JD2418035
TT Aql P = 13.7518d. Current elements - see Table.
TV Aql P var (changed at ~JD2430000).
TV Aql Before JD2430000 Max = 2429730 + 237.9d*E.
TW Aql Cycles 65d or 95d are observed during different time
TW Aql intervals [8714].
UU Aql Mean cycle: 71.3d [4063]; 56d [3144].
UY Aql Cyclic changes of light (P ~400d) with superimposed very
UY Aql rapid variations are noted in [0504].
VX Aql SC5-/8e. According to [4231], the variable is irregular.
VX Aql Lithium star.
VZ Aql B - V: +0.61, +1.01.
XZ Aql P var. Min = 2424449.277 + 2.139147d*E
XZ Aql (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],
AD Aql the range is 8.83 - 13.42 V.
AE Aql VB A (B 16.6m, 12", 330deg; C 16.9m, 11", 0deg).
AE Aql The combined light of A, B, C varies in the range
AE Aql 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 -
BL Aql 29075). During JD2436420 - 38940 - see Table.
BY Aql P var?
CD Aql Close companion?
CL Aql Sometimes maxima predicted according to the
CL Aql elements do not occur.
CM Aql Symbiotic spectrum similar to that of Z And [3149].
CR Aql Considerable Blazhko effect is possible.
CS Aql Close companion?
CT Aql According to [6004], only slow irregular variations with
CT Aql Delta(m) ~0.6 were observed in 1963 - 1968.
CU Aql P var? (Possible change ~JD2423000). Earlier Max = 2418591
CU Aql + 203.7d*E.
CV Aql P var?
CW Aql Close companion?
DD Aql Close companion?
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). SB1 (P = 1435d).
FG Aql At the edge of the dark nebula Barnard 130. May be a
FG Aql physical pair with FH Aql (rho ~20"). According to
FG Aql [0504], the mean cycle of light variations is 3.5d.
FG Aql The level of mean light varies.
FH Aql At the edge of the dark nebula Barnard 130. May be a
FH Aql physical pair with FG Aql (rho ~ 20"). According to
FH Aql [0504], the mean cycle of light variations is 3.44d.
FK Aql Depth 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
HL Aql co-ordinates coincident with those given at the discovery
HL Aql is constant according 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 VB B (A = 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 +
KO Aql 2.863859d*E (JD2426250 - 33000) [2462]; Min =
KO Aql 2433888.366 + 2.863954d*E (JD2433000 - 39000).
KO Aql 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.
KV Aql During JD2428308 - 28433 the star was faint. Max 2436015
KV Aql also is not satisfied by the elements.
LU Aql In [3158] P = 102d is given, and the existence of the
LU Aql variation of mean magnitude with P ~1080d and
LU Aql 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
NV Aql Delta(m) ~0.6m.
OO Aql Min II 9.8. P var. Min I = 2426892.0582 +
OO Aql 0.5067954d*E (1932 - 1934), Min I = 2433925.3762 +
OO Aql 0.5067943d*E [8072]. Since JD2438000 - see Table.
OO Aql 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
PP Aql is not excluded. According to [3161]
PP Aql P var. Max = 2415229.15 + 24.0147d*E (JD2415228 -
PP Aql 21064), Max = 2426576.14 + 24.074d*E (JD2426576 -
PP Aql 29489). After JD2432040 Max = 2433141.78 + 23.994d*E.
PP Aql Current elements Max = 2436836.04 + 23.973d*E.
PZ Aql P var? According to [5387], before JD2428075 P = 8.7555d;
PZ Aql P = 8.7504d (JD2428075 - 34725); since JD2434725
PZ Aql P = 8.7573d. See also [2274]. Elements in the Table are
PZ Aql satisfactory after JD2433150. The shape of the light curve
PZ Aql 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?
V0336 Aql B - V: +1.17, +1.55.
V0337 Aql Min II 9.09. P var.
V0337 Aql The shape of the light curve varies.
V0340 Aql d = 0.05P. P var.
V0341 Aql P var. Delta(S) = 4.
V0342 Aql ADS 12259 B (A 7.5m; B 20", 14deg); d = 0.032P. P
V0342 Aql increases (see also [2265, 4493]). Before JD2435600 Min =
V0342 Aql 2428023.550 + 3.390842d*E.
V0342 Aql Halpha emission observed at Max light [8074]. The shape
V0342 Aql of the light curve and d apparently vary. Delta(m)
V0342 Aql probably decreases [8075].
V0343 Aql Min II 10.7.
V0346 Aql Min II 9.1. ADS 13438 A (B 11.3m, 2", 245deg).
V0346 Aql Elements in the Table are valid after
V0346 Aql JD2437000. The shape of Min I varies [7001].
V0348 Aql d ~0.08P.
V0352 Aql The nucleus of the supposed planetary nebula P.K.
V0352 Aql 37-3.3deg.
V0356 Aql VB A (B 0.2").
V0367 Aql The elements are satisfactory
V0367 Aql only during JD2436450 - 37960. Resembles S Vul.
V0368 Aql VB A (B 0.17", 140deg).
V0374 Aql VB A (B ~0.2', ~270deg).
V0406 Aql Min II 13.3:.
V0407 Aql P var; there is a nonlinear term in the elements:
V0407 Aql +1.51d*10**(-9)*E**2.
V0409 Aql Min II 12.2. Spectral type from another publication
V0409 Aql is A2 - A3.
V0411 Aql Epoch of Min is given.
V0417 Aql Min II 11.5. P var. Before JD2439000:
V0417 Aql Min = 2428427.127 + 0.3701251d*E.
V0421 Aql P var?
V0423 Aql Elements are valid for JD2426900 - 28000. During
V0423 Aql JD2429020 - 31670 the waves are much longer or absent.
V0433 Aql Waves of 26d - 80d duration with Delta(m) = 0.1m - 0.9m.
V0433 Aql The mean light varies according to the formula
V0433 Aql Max = 2438312 + 648d*E.
V0449 Aql The star in [1091, 2282] is actually not identical to HV5424.
V0461 Aql Close component ~15.5m, the range of combined light is
V0461 Aql given.
V0467 Aql Waves of 40d - 72d duration. The mean light varies with
V0467 Aql P ~1400d.
V0473 Aql P ~330d is sometimes observed.
V0476 Aql EW type with doubled period is possible. Elements are based
V0476 Aql on a short series of observations.
V0483 Aql In the field of the open cluster NGC 6709.
V0486 Aql In the field of the open cluster NGC 6709.
V0493 Aql B - V: +1.10, +1.38.
V0495 Aql d = 0.06P:.
V0496 Aql B - V: +1.07, +1.28. Elements are given for epochs after
V0496 Aql JD2428000.
V0497 Aql VB A (B 16.5m, 9", ~0deg).
V0524 Aql The variable is np from the star shown in the chart
V0524 Aql in [2317].
V0527 Aql IS type is possible.
V0528 Aql VB A (B 16.5m, 11", 59deg).
V0535 Aql VB [1943], two components are seen on Palomar prints,
V0535 Aql eastern of them being red. According to [1943], rapid
V0535 Aql variable.
V0537 Aql Possible P = 200d.
V0538 Aql Possible P = 375d.
V0558 Aql Possible P = 187d.
V0571 Aql Possible P = 185.5d.
V0572 Aql B - V: +0.65, +0.87. P var. Before JD2435500 P ~3.7686d.
V0572 Aql See also [8637]. JD2433631.8421 + 0.716292d*E.
V0572 Aql See also [2124].
V0586 Aql Irregularities are sometimes observed, but then the
V0586 Aql periodicity is probably resumed.
V0596 Aql Resembles S Vul.
V0599 Aql Min II 6.73. According to [8083], may be constant.
V0600 Aql B - V: +1.36, +1.70.
V0600 Aql Before JD2428000 another value of P is possible [8632].
V0602 Aql d = 0.02P. Min II 12.7.
V0603 Aql SB (P = 0.13854d [3169]). Outside the outburst there are
V0603 Aql variations of light (eclipses) with Delta(m) = 0.30m,
V0603 Aql Min I = 2444401.399 + 0.1377d*E (D ~0.2P). The
V0603 Aql shape of the light curve and the depth of minima differ
V0603 Aql from cycle to cycle. The brightness in minima shows
V0603 Aql fluctuations apparently connected with the presence of
V0603 Aql a hot spot [4500].
V0605 Aql A unigue variable. 8" np from a 17m star. Min ~20m pg.
V0605 Aql Photographs of the field [6041, 6042]. The
V0605 Aql light curve resembles those of the SN in NGC
V0605 Aql 1058 or of eta Car [6040]. The only Max observed, with
V0605 Aql fluctuations, occured in 1918 - 1924. In 1921 the spectral
V0605 Aql type was found to be R [2464]. The star is inside the old
V0605 Aql planetary nebula A 58 and may be its nucleus.
V0609 Aql Min II 11.9.
V0615 Aql P var? Max = 2428046 + 364d*E (JD2428038 - 31343) [1091].
V0616 Aql d = 0.04P. Elements reguire verification.
V0618 Aql Twice shorter period is not excluded.
V0637 Aql Twice shorter period is not excluded.
V0638 Aql Twice shorter period is not excluded.
V0640 Aql Min II 12.8.
V0647 Aql Slight Min II [1091].
V0663 Aql P = 194.5d is possible.
V0666 Aql The range is given for combined magnitude with a preceding
V0666 Aql 16.5m star. Separately was found ~17m pg near Min.
V0672 Aql P var? Blazhko effect is possible [3113].
V0678 Aql P var. Before JD2429723 Max = 2429723 + 120.6d*E.
V0688 Aql Min II 10.8. DII = 0.15P.
V0694 Aql d = 0.13P. VB (1"), a companion ~1m fainter than
V0694 Aql the variable [1881] may have affected the data given.
V0699 Aql Min II 13.75.
V0706 Aql Delta(S) = 0:.
V0708 Aql P ~65d waves superimposed on slow variation of mean
V0708 Aql brightness with P ~1350d (JD2437124 - 40512) [6025].
V0708 Aql According to [0773] waves with P ~100d - 150d
V0708 Aql (JD2427543 - 31318).
V0714 Aql d = 0.05P.
V0724 Aql Min II 11.57.
V0733 Aql P var? Before JD2434500,
V0733 Aql possibly Max = 2434453.72 + 6.17687d*E [0001].
V0734 Aql VB A? (B 16.1m?).
V0743 Aql White. SRD?
V0755 Aql Alternative elements: Min = 2429195.290 + 1.01598d*E.
V0765 Aql B - V: +0.70, +0.80.
V0766 Aql EW type is not excluded.
V0769 Aql d = 0.05P?
V0770 Aql Min II 14.0.
V0771 Aql According to [3165] UG.
V0774 Aql Possibly resembles UV Boo.
V0777 Aql P = 111.5d is possible.
V0784 Aql Min II 14.8.
V0794 Aql Rapid changes with Delta(m) up to 1.5m superimposed on
V0794 Aql slow ones. May belong to "polars" of XPRM type. Peculiar
V0794 Aql spectrum with broad emissions and blue continuum [8676].
V0800 Aql VB. According to [6072] UGZ.
V0801 Aql VB A (B 15.1m sp).
V0803 Aql Min II 14.8.
V0804 Aql Min II 12.8. In Max B - V = +0.61.
V0805 Aql Min II 7.90, DII = 0.11P.
V0808 Aql Min II 13.3.
V0812 Aql VB A (B 16m sp, C 16m sf).
V0814 Aql VB A (B 16.5m sp).
V0822 Aql Min II 7.07. ADS 12538 A (B 10.1m, 1", 67deg). The shape
V0822 Aql of the light curve varies.(U - B) index in Min I is redder
V0822 Aql and Min II is bluer than average.
V0829 Aql Twice longer P is possible.
V0836 Aql RR type is possible ([0085]; it is suggested also by the
V0836 Aql spectrum [8676]).
V0850 Aql In the centre of the planetary nebula P.K. 37-6.2.
V0866 Aql Min II 14.8. According to [6026], the depth
V0866 Aql of Min II 0.4m, EB type.
V0867 Aql P var?
V0871 Aql Min II 14.5, Min II - Min I = 0.425P.
V0871 Aql Physical changes in the range 13.3 - 13.6 are
V0871 Aql possible. Eclipses start from the 13.6m level.
V0872 Aql Min II 15.7:. Apsidal motion is possible.
V0873 Aql P var? The mean light varies in the range 13.8 - 14.0.
V0875 Aql White. According to [6004], rapid. Possibly UGZ or IA.
V0877 Aql VB A (B 16.5m nf).
V0882 Aql Blazhko effect is possible.
V0885 Aql Min II 14.9:. Apsidal motion and changes of the shape of
V0885 Aql the light curve are possible.
V0888 Aql A possible member of the open cluster NGC 6738.
V0889 Aql Min II 9.0. Min II - Min I = 0.35P.
V0889 Aql Apsidal motion is possible.
V0890 Aql Nova Aql 1946 = asteroid N258 Tyche [9038].
V0891 Aql Min II 15.8.
V0895 Aql P var. Max = 2430931.435 + 0.265108d*E
V0895 Aql (JD2426920 - 35010) [2267].
V0895 Aql During JD2441890 - 42290 - see Table.
V0907 Aql Min II 15.7.
V0912 Aql The shape of the light curve varies.
V0914 Aql P = 3.336217d
V0914 Aql is given in [8717] by misprint.
V0919 Aql Min II 13.8.
V0920 Aql F or earlier observations Max = 2429458.400 + 0.4955033d*E.
V0922 Aql Elements are not quite reliable.
V0923 Aql Unusual shell star [1884]. Similar to EW Lac.
V0923 Aql He lines are widened by the rotation, NaI lines
V0923 Aql are narrow. Light changes are periodic: Min =
V0923 Aql 2436458.66 + 0.8518d*E. The cause of variations is
V0923 Aql probably connected with the rotation and the inhomogeneous
V0923 Aql brightness distribution over the disk of the star [3178].
V0923 Aql Profiles of spectral lines vary. The expansion of the
V0923 Aql envelope terminated in 1965, which apparently led to the
V0923 Aql development of inhomogeneities and to the broadening of
V0923 Aql hydrogen line profiles [4525].
V0925 Aql Some observers found constant brightness [3165].
V0929 Aql Short period.
V0936 Aql Short period.
V0947 Aql According to [5412], rapid irregular
V0947 Aql changes are not excluded. According to [0504], constant.
V0955 Aql Min II 14.9, DII = 0.13P.
V0956 Aql Min II 14.2. Elements need confirmation.
V0957 Aql P var. Max = 2428154.960 + 0.6051327d*E
V0957 Aql (JD2421871 - 28105).
V0958 Aql VB A (B 17.0m, 0.2' np; C slightly brighter, 0.1'f).
V0958 Aql Combined magnitude of A and C is given.
V0964 Aql Min II 13.7.
V0969 Aql Blazhko effect is possible.
V0981 Aql Min II 14.5.
V0991 Aql IS type is possible.
V0992 Aql According to [4260], P = 110d.
V0998 Aql The position coincides with the planetary nebula
V0998 Aql P.K.50-3.1deg.
V0999 Aql Tsessevich's observations [7806] do not agree with the
V0999 Aql elements in the Table.
V1017 Aql Elements need confirmation.
V1033 Aql P var?
V1045 Aql Min II 13.5.
V1046 Aql P var? [8321].Min = 2427713.314 + 5.28303d*E [4027].
V1046 Aql Slight reflection effect is possible.
V1064 Aql Cycles 295d - 410d.
V1072 Aql sp component of a close pair.
V1075 Aql d = 0.04P. Min II 13.6.
V1076 Aql VB A (close preceding).
V1086 Aql VB. Probably the variable is the sf component.
V1093 Aql IA type is possible.
V1095 Aql P var. After JD2429048 - see Table, earlier
V1095 Aql Max = 2427322 + 42.68d*E. Not coloured appreciably.
V1096 Aql Min II 13.3.
V1097 Aql Min II 14.0.
V1101 Aql Possibly UGZ type [3156].
V1113 Aql The period may be twice shorter.
V1117 Aql Min II 16.6.
V1125 Aql Min II 16.0.
V1140 Aql P var?
V1154 Aql Min II 14.8; Min II - Min I = 0.70P.
V1165 Aql According to [4564], constant. In [3932] was not separated
V1165 Aql from a close component which probably led to distortions
V1165 Aql of the light curve.
V1166 Aql UG type is possible.
V1173 Aql nf component of a close pair.
V1182 Aql Min II 8.65.
V1184 Aql Min II 13.4.
V1200 Aql VB. The variable is the eastern red component.
V1204 Aql VB. The variable is the eastern component.
V1208 Aql A common proper motion star 9.06m in 1' to the south.
V1248 Aql UG type is possible.
V1251 Aql Red.
V1261 Aql Spectral type K2 in HD.
V1269 Aql VB. The variable is the preceding component.
V1281 Aql Reddish. SRD type is possible.
V1286 Aql Possibly the period is accidental.
V1288 Aql ADS 12182 A (B 12.3m, 36", 287deg).
V1291 Aql The elements have been determined on the base of magnetic
V1291 Aql field variations. The epoch of minimum intensity of the
V1291 Aql magnetic field is given.
V1295 Aql Shell star. Dramatic spectral changes were observed [5240].
V1295 Aql The variability is hardly periodic, though P ~100d is
V1295 Aql possible. Sometimes light fluctuations on several days'
V1295 Aql time scale are observed [5880]. IR excess [6277]. For a
V1295 Aql detailed spectroscoric study, with evidence for the
V1295 Aql outflow of matter from the surface, see [4739].
V1295 Aql Considerable magnetic field [4435].
V1297 Aql d = 0.05P? Min II 14.5.
V1298 Aql mu alpha = -0.0392s, mu delta = -1".330.
V1298 Aql The companion of the star BD +4deg 4048 (ro =
V1298 Aql 73".8, theta = 151.5 deg).
V1298 Aql One of the absolutely faintest known stars (Mv = +19m).
V1300 Aql I - K: +5.2, +6.5. Sometimes CO, SiO, OH maser emission.
V1302 Aql A unique IR object IRC +10420. B - V = +2.7, U - B = +1.9.
V1302 Aql OH, H2O, SiO maser. According to [7437], the energy
V1302 Aql distribution in the IR spectrum (1 - 22mkm) resembles that
V1302 Aql of eta Car. Emissions of neutral metals are observed in
V1302 Aql the spectrum. Increased in brightness during 1925 - 1970;
V1302 Aql Max ~1970.
V1323 Aql Close VB; var - northern component.
V1325 Aql VB, np component var.
V1325 Aql VB, np component var.
V1331 Aql Min II 7.95. According to [4619] P = 1.364076d.
V1333 Aql Aql X-1. Light variations with P ~1.28d - 1.31d due to
V1333 Aql orbital motion are possible [4625]. Bursts characteristic
V1333 Aql of the XB type are observed [4757]. Lx/Lopt ~500 outside
V1333 Aql nova-like bursts, Lx/Lopt ~5000 during bursts.
V1336 Aql In 1.6' W from MXB 1916-05. M type is possible.
V1338 Aql VB. Probably the f component, very bright infrared, is var.
V1340 Aql d = 0.06P? Intrinsic lightvariations in Max are possible.
V1341 Aql Min II 13.4. P = 0.3586768D is possible.
V1343 Aql SS 433. = +2.0. Associated with the SNR W 50. Mean
V1343 Aql light varies in the range 14.0 - 14.6 V according to the
V1343 Aql elements Max = 2443662.5 + 165.5d*E [0512]. The depth of
V1343 Aql Min I varies from 0.2m to 0.9m V, the depth of Min II
V1343 Aql varies from 0 to 0.4m V. Two systems of H, HeI, HeII
V1343 Aql emission lines are observed in the spectrum: the
V1343 Aql "stationary" system corresponding to Vr changes from 300
V1343 Aql to 150 km/s with P = 13.1d, and the "relativistic" one,
V1343 Aql corresponding to Vr changes from +50000 to -35000 km/s
V1343 Aql with P = 165.5d. The spectral study [0535]. The system
V1343 Aql apparently consists of an O - B star filling its inner
V1343 Aql Roche lobe and a compact object surrounded by an accretion
V1343 Aql disc wich is precessing with P = 165.5d. Two jets
V1343 Aql consisting of dense condensations of matter emerge from
V1343 Aql the system with relativistic velocity (0.27 c) in opposite
V1343 Aql directions. The luminosity of the disc amounts to not less
V1343 Aql than 60% of the total luminosity of the system [0926, 0953].
V1343 Aql The object may be a former supernova which bursted not
V1343 Aql more than 10**4 years ago.
V1345 Aql Min II 14.3:, Min II - Min I = 0.46P.
V1349 Aql Max ~17 pg.
V1352 Aql VB A (B 14.5m, 6", 175deg).
V1353 Aql Min II 10.9.
V1355 Aql Min II 13.3.
V1357 Aql Possibly P = 1.051d.
V1470 Aql The variability may be due to the fainter (B) component.
V1472 Aql SB, Porb = 198d.
eta Aql P var. P = 7.176344d (JD2373000 - 95100),
eta Aql P = 7.176455D (JD2395100 - 2412100). Since JD2412100 -
eta Aql see Table. For the whole interval
eta Aql Max = 2442794.773 + 7.176735d*E + 2.18d*10**(-8)*E**2
eta Aql [8632]. In the UV band the light of a possible A0V
eta Aql comparion is apparent.
sig Aql ADS 12737 A (B 12.34m, 48", 328deg). Depth of Min II 0.1m.
sig Aql In [4627] P = 1.950271d is given according to
sig Aql spectroscopic 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 +
S Ara 0.45188910d*E (JD2414000 - 19000);Max =
S Ara 2419149.797 + 0.45188581d*E (JD2419000 -
S Ara 30000) [0752]. Since JD2441000 - see Table. For the
S Ara whole interval, with sufficient accuracy,
S Ara Max = 2420047.2382 + 0.451888176d*E - 1.36d*10**(-10)*E**2
S Ara [3126].
T Ara VB A (B 11.0m, 34", 60deg).
X Ara Shown in the chart for S5809.
RT Ara According to Cannon [1944] who discovered the star's
RT Ara variability, a companion 12.0m is present in 0.1m to W
RT Ara and somewhat to the north from the variable. Cannon points
RT Ara out that at Min light the variable becomes fainter than
RT Ara the companion. No sign of the companion's existence was
RT Ara found by Hoffmeister [0016] and by Payne-Gaposchkin [0624].
RT Ara According to [0624], the mean cycle is ~78d, and RVA
RT Ara type is possible.
RW Ara d = 0.022P. Min II 8.91. Changes of the shape of the light
RW Ara 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
YY Ara 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.
AE Ara A compast planetary nebula or a symbiotic star. Irregular
AE Ara abrupt brightenings by 3m - 4m separated by several years
AE Ara are observed [0255]. The spectral data are discussed in
AE Ara [8076].
AF Ara Min II 13.8.
AW Ara Before JD2417300 Max = 2412600 + 186d*E.
BQ Ara Double maxima separated by 10d - 20d, with Min II 12.8.
CC Ara VB; the variable is nf component.
CH Ara Noted on the finding chart for S6062 = V 466 Ara.
CT Ara Before JD2420400 Max = 2413080 + 215d:*E;
CT Ara since JD2425000 - see Table.
DU Ara B - V: +0.52, +0.84. P var. Max = 2418145.560 +
DU Ara 1.63999d*E (JD2411000 - 21000); Since
DU Ara JD2425000 - see Table.
EK Ara VB A (B 15m).
EL Ara Before JD2420400 Max = 2415140 + 332d*E;
EL Ara since JD2425000 - see Table.
ER Ara Min II 14.2.
EV Ara Before JD2420400 Max = 2413750 + 237d*E;
EV Ara since JD2425000 - see Table.
EZ Ara P var.
FU Ara The depth of Min I is 0.97m and 0.89m,
FU Ara the depth of Min II is 0.20m and 0.23m in blue and
FU Ara yellow light, respectively.
GK Ara Before JD2417800 Max = 2414050 + 237d*E,
GK Ara since JD2418400 - see Table.
GM Ara Min II 12.8.
HX Ara B - V: +0.23, +0.36. A hump on the ascending branch
HX Ara (phi = 0.93P) [8118].
KY Ara Only one sharp Max (JD2428715 - 712) was observed.
KY Ara 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
LQ Ara 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 variable is np component of the pair.
QX Ara Shown in the chart for S5818.
V0340 Ara B - V: +1.25, +1.68. [A/H] = 0.6.
V0341 Ara The star is blue; light variations during 4d were not
V0341 Ara accompanied by colour changes. Possibly an eclipsing
V0341 Ara variable [4678].
V0342 Ara P >= 140d.
V0344 Ara P >= 170d
V0345 Ara P >= 180d.
V0349 Ara Min II 8.8.
V0355 Ara P > 220d.
V0356 Ara P > 170d.
V0357 Ara P >= 220d.
V0360 Ara Min II 13.8:, Min II - Min I = 0.35P.
V0361 Ara Min II 13.6:.
V0362 Ara Min II 15.6:.
V0383 Ara A star 16.5m is close to the north.
V0421 Ara Min II 15.1.
V0440 Ara Min II 14.5:.
V0444 Ara Min II 14.2.
V0454 Ara Min II 14.1.
V0480 Ara Min II 15.5:.
V0484 Ara RV type is possible (Min = JD2436760).
V0485 Ara Min II 14.8.
V0489 Ara Min II 11.9.
V0491 Ara Min II 11.9.
V0492 Ara Min II 14.5.
V0494 Ara RV type is not excluded.
V0501 Ara Min II 13.8. Shown in the chart for S6114.
V0535 Ara Min II 7.71. Nonlinear term in the elements:
V0535 Ara -4.4d*10**(-11)*E**2.
V0536 Ara Min II is present. EB type is possible. P var.
V0536 Ara P = 2.374101d (JD2415000 - 22000); since JD2422000 -
V0536 Ara see Table.
V0539 Ara VB A (B 9.22m, 12", 269deg). Min II 6.09, d = 0.01P.
V0539 Ara Shown in the chart for BV1441 = V538 Ara.
V0544 Ara 14.5m star sp.
V0609 Ara Shown in the chart for S5867.
V0610 Ara EA type is possible.
V0613 Ara VB (close np companion is NSV10198).
V0616 Ara Deep Min II.
V0620 Ara Min II is possibly present.
V0623 Ara Min II 14.5. Twice shorter period is possible.
V0624 Ara P >= 220d.
V0625 Ara P >= 170d.
V0639 Ara V1 (NGC 6397). Probably not a cluster member.
V0651 Ara Min II 15.3.
V0653 Ara Min II 12.6.
V0656 Ara EW type is not excluded.
V0658 Ara Min II 16.0.
V0659 Ara Min II 14.4.
V0668 Ara Min II 13.8:.
V0675 Ara P >= 200d.
V0687 Ara RRC type is possible.
V0700 Ara Min II 15.7.
V0702 Ara Min II 14.0.
V0704 Ara Min II 13.3.
V0705 Ara Min II 14.4. RR type is possible.
V0716 Ara Monotonous brightening during JD2436689 - 36838 was
V0716 Ara found. The amplitude is probably greater.
V0722 Ara Min II 10.3:.
V0728 Ara Min II 12.8.
V0732 Ara CEP type is not excluded.
V0743 Ara RV type is possible.
V0781 Ara Min II 14.8:.
V0783 Ara Min II 13.9:.
V0785 Ara Min II 14.3.
V0787 Ara RV type is possible. Min JD2436756.
V0789 Ara Min II 14.8.
V0790 Ara Min II 14.8.
V0791 Ara Min II 13.0:.
V0792 Ara Min II 15.2:.
V0801 Ara MXB 1636-53. Description of the spectrum [1356].
V0801 Ara Modulation with P ~4h and the amplitude up to 40% was
V0801 Ara found in the broad band optical flux [4944].
V0802 Ara 14.93 - 17.03 B.
V0808 Ara EW type is possible.
V0820 Ara Epoch of Min is given. Strong magnetic field. Either an
V0820 Ara eclipsing binary or (more probably) an object similar to
V0820 Ara rotating variables of ACV type.
V0821 Ara 4U 1658-48. Unusua1 X-ray system. Quasiperiodic optical
V0821 Ara variations (P ~20s) with total amplitude 40 percent,
V0821 Ara abrupt bursts on ~20 ms time scale leading to two-fold
V0821 Ara flux increase and light changes by 6m during less than
V0821 Ara two months were observed [4958]. Lx/Lopt = 3.
V0870 Ara Type DSCT: is also possible.
R Ari OH emission.
T Ari P var. Max = 2417160 + 313.5d*E (JD2404800 -
T Ari 17200); Max = 2434616 + 323.1d*E (JD2419400 -
T Ari 34560). Since JD2436560 - see Table. = 319.53d
T Ari (JD2404800 - 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 +
X Ari 0.6511248d*E (JD2420460 - 33210) [3506]. Since
X Ari JD2433210 - see Table. [Fe/H] = -2.17.
RR Ari Min II 6.75:; Min II - Min I = 0.55P. Variability is not
RR Ari confirmed by other authors' photoelectric observations.
RR Ari 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.
RV Ari P1 = 0.07195d [8137]; P2 = 0.27554d [7033]. Moments of
RV Ari brightest light maxima T = 2435066.400 + 0.31632996d*n
RV Ari [2290].
RW Ari B - V: +0.35, +0.46. P var. Max = 2428183.324 +
RW Ari 0.3543184d*E (JD2428040 - 36700) [3188]. Since
RW Ari JD2440900 - see Table. According to [6043] - EA type:
RW Ari Min I = 2439384.97 + 3.1754d*E. Total light range
RW Ari (11.47 - 13.25 V) [8127] seems doubtful. It is not
RW Ari excluded that the eclipses and light increase of RW Ari
RW Ari given in [8127] are explained by variability of one of
RW Ari 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 =
ST Ari 2429525 + 106.6d*E (1939 - 1942); Max = 2430588 +
ST Ari 95.2d*E (1942 - 1946); Max = 2432118 + 100.0d*E
ST Ari (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
TT Ari typical for Z Cam variables there are sinusoidal variations
TT Ari with amplitude of about 0.2m B and variable period:
TT Ari P = 0.1329d (1961 - 62), P = 0.1327d (1966) [4931],
TT Ari P = 0.1326d (1978) [4935]. Sinusoidal variations are
TT Ari superimposed by quasiperiodic oscillations up to 0.2m with
TT Ari 8 - 20 minutes cycle and irregular flickering up to 0.1m
TT Ari in 1 minute.
TU Ari P var. Max = 2420463.353 + 0.4716219d*E
TU Ari (JD2420463 - 34720). Since JD2436820 - see Table.
TV Ari P var.
TX Ari P var?
TY Ari Form of the light curve varies. Mean value of the period
TY Ari is given.
UV Ari The second overtone period given in the
UV Ari Table is dominating. Sometimes the fundamental
UV Ari period P0 = 0.062d and the first overtone period P1 =
UV Ari 0.047d are observed.
UW Ari Amplitude varies. In the interval JD2441581 - 693 - const.
UW Ari [7544].
UX Ari T = 2440133.766 + 6.43791d*E [6444], where T is epoch of
UX Ari conjunction (G5 component is behind K0 component).
UX Ari Brightness varies in waves with a period ~Porb, but the
UX Ari phase psi of light minimum calculated according to the
UX Ari elements given above changes with time: psi = 0.1P
UX Ari (1972 - 1974), psi = 0.8P (1976), psi = 0.7P (1977),
UX Ari psi = 0.6P (1978). Mean brightness varies, amplitude of
UX Ari the wave varies from 0.04m up to 0.15m.
VW Ari BDS 1269 A (B 8.33m, 74", 31deg). P2 = 0.089d.
VW Ari Metal deficiency. The companion has normal metal abundance.
VY Ari SB? Epoch of Min is given.
VY Ari Second light variation is also observed: Min =
VY Ari 2442044.6 + 43.9d*E. A small flare in U band was
VY Ari 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];
R Aur cycle 64.5a is possible.
S Aur P var. In the early fourties of our century the star was
S Aur faint with small and irregular variations.
T Aur Min = 2437614.0088 + 0.20437851d*E [8145]. P var?
T Aur = 14.92, = + 0.28. There are light
T Aur fluctuations between the eclipses. Depths of Min are
T Aur 0.10m - 0.28m [3195]. Faint nebula with high degree of
T Aur ionization.
U Aur H2O maser.
Y Aur B - V: +0.70, +1.06.
Z Aur P var [7110]. Max = 2425580 + 110.76d*E
Z Aur (JD2416156 - 25580); Max = 2429888 + 113.35d*E
Z Aur (JD2425570 - 29900); Max = 2438292 + 135.55d*E
Z Aur (JD2429900 - 33300). P = 110d (1965) [3196].
Z Aur In 1970 - irregular variations [7338]. = -165 km/s;
Z Aur 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 =
RT Aur 2433040.867 + 3.728365d*E (JD2417970 - 33100).
RT Aur Since JD2433100 - see Table. Delta(V) var?
RU Aur OH emission.
RU Aur Mean magnitude probably varies with Pi = 10400d [1059].
RV Aur VB A (B 12.5m, dM0e, 1.2", 254deg).
RV Aur The companion probably flares with an amplitude
RV Aur 0.5m - 0.7m [3197, 3198]. Possible period of axial
RV Aur rotation is 100d [7067]. OH emission.
RX Aur B - V: +0.76, +1.18; [A/H] = -0.1, P var?
RX Aur Nonlinear term: -0.70d*10**(-6)E**2?
RZ Aur P var. Min = 2422616.498 + 3.010593d*E
RZ Aur (JD2418000 - 26000); since JD2426000 - see Table.
SS Aur SB (P = 0.1805939d [6103]).
SS Aur Sometimes abnormal behaviour of the star is
SS Aur being observed when comparatively numerous and
SS Aur small light maxima arise. According to [8151] the
SS Aur mean cycle is 51.2d.
SU Aur Common proper motion with AB Aur (P = 3'). Associated
SU Aur with a small bright nebula. OH emission.
SX Aur Min II 8.87. According to [8153] P var:
SX Aur 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].
SY Aur Max = 2436853.57 + 10.144330d*E (JD2417900 -
SY Aur 32380). Since JD2432380 - see Table.
TT Aur Min II 9.0.
TV Aur S5/6-.
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).
UV Aur 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 Common proper motion with AB Aur (P = 3'). Associated
AB Aur with a small bright nebula. OH emission. Spectrum
AB Aur description [4002].
AE Aur Connected with the bright nebula IC
AE Aur 405. The motion is directed away from Ori OB 1
AE Aur association with the velocity 106 km/s.
AG Aur According to TiO bands
AG Aur 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:
AK Aur +0.18.
AM Aur Min II 11.0. P var: Min I = 2417617.2 + 13.6182d*E
AM Aur (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
AP Aur (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 =
AR Aur 2427887.7217 + 4.13467d*E (JD2427800 - 29500) [4999].
AR Aur Since JD2438400 - elements in the Table with an additional
AR Aur 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 +
BF Aur 1.583217d*E (JD2411760 - 34455) [5038]. Since JD2434455
BF Aur - see Table. The two sets of observations are equally well
BF Aur represented by the formula: Min I =
BF Aur 2440628.3643 + 1.5832212d*E + 1.7d*10**(-10)*E**2 [8160].
BH Aur P var. Max = 2437352.461 + 0.45608821d*E (JD2417260 -
BH Aur 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 =
CI Aur 2439414.573 + 1.869984d*E + 0.020d*10**(-8)*E**2
CI Aur (JD2425560 - 42045). Elements given in the Table represent
CI Aur observations in the interval JD2439052 - 40654.
CL Aur Min II 12.3; Min II - Min I = 0.45P; DII = 0.13P. P var?
CL Aur Min I = 2432967.262 + 1.2443666d*E (JD2416900 - 32967)
CL Aur [0608]. Since JD2432967 - see Table.
CO Aur The first overtone period is
CO Aur 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 =
CQ Aur 0.52P:; D = 0.096P. P var. Nonlinear term:
CQ Aur +3.78d*10**(-7)*E**2.
CY Aur [A/H] = -0.3.
DV Aur P var. Max = 2426015 + 198.0d*E (JD2426014 - 27400) [0332].
DV Aur 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
ER Aur (1949 - 1950) [1059]. In the interval JD2443428 - 874 -
ER Aur 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 -
GO Aur 31325); Max = 2432205 + 301.2d*E (JD2432805 -
GO Aur 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.
HN Aur Light variations with P2 = 1400d: are
HN Aur superimposed by variations with P1 = 165d:.
HP Aur Min II 11.28; Min II - Min I = 0.502P. P var. Min I =
HP Aur 2427445.400 + 1.4228180d*E (JD2427445 - 42683); since
HP Aur 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
HS Aur doubled as the system consists of two equal components
HS Aur [8164].
HU Aur Min II 12.4.
HW Aur Min II 12.6.
HZ Aur Sometimes short period variations of Vr with the amplitude
HZ Aur 3 km/s and of brightness in U with the amplitude 0.02m are
HZ Aur also observed. Max Vr = 2439454.900 + 0.073502d*E
HZ Aur [5259]. P (DeltaU) = 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.
IS Aur It is not known which of the components varies.
IU Aur P var. There is an additional periodic term in the elements:
IU Aur -0.00627d*sin (2.221deg*E + 15deg). The ratio of Min II
IU Aur depth to Min I depth is 0.78. There is secular deepening
IU Aur of both minima. The depth of Min I increases by 0.016m per
IU Aur year. The range of light variation in the Table is given
IU Aur for 1979.0 (Min II 8.69). Orbital inclination is increasing
IU Aur by 0.5deg per year [5181] due to orbital precession caused
IU Aur by a third body. Spectrum description [8166].
KO Aur Min II 11.2.
KR Aur = +0.10, = -0.95. SB (P = 0.1628d [9045]).
KR Aur Spectrum description [8169, 8170]. Wide hydrogen emission
KR Aur lines. Long maxima and minima lasting for years are
KR Aur superimposed by rapid light variations by 1 - 2m in
KR Aur several days or fortnights and by 0.5m in dozens of
KR Aur 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 sometimes
KV Aur superimposed by comparatively rapid fluctuations.
KW Aur VB A (B 11.0m, 11.1", 352deg, 1909; C 7.99m, 14.5",
KW Aur 226deg, 1923); SB1 (P = 3.788568d). Mean light level
KW Aur varies synchronously with orbital motion. Besides main
KW Aur pulsational period there are two more periods of nonradial
KW Aur pulsation: P1 = 0.096533d, P2 = 0.088243d.
KX Aur In the IC 405 nebula.
KY Aur In the IC 405 nebula.
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.
NW Aur According to [7160] no minimum was recorded during
NW Aur 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.
OX Aur Mean brightness probably varies.
PR Aur The chart in [7806] is wrong.
PY Aur Possibly a cepheid.
QR Aur Epoch of Min is given.
QY Aur SB.
V0348 Aur VB A (B 13.43m, 24", 44deg).
V0353 Aur During several decades the star brightened by 0.06m in a
V0353 Aur year. Possibly a planetary nebula in the process of
V0353 Aur formation.
V0358 Aur In the region of the cluster NGC 2099.
V0431 Aur P = 16.86d detected in HIPPARCOS data.
V0433 Aur SB?
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.
eps Aur Survey of the physical properties of the system [2041,
eps Aur 2042, 3070, 3216, 3217, 8174]. The spectrum probably
eps Aur varies even outside eclipses. The eclipses are probably
eps Aur due to a disk of gas and dust surrounding the hot
eps Aur companion. The brightness has physical fluctuations
eps Aur with the amplitude up to 0.24m and the cycle about 110d
eps Aur [2040] which hinder revealing the possible Min II.
eps Aur Similar cycle was discovered also in the fluctuations
eps Aur of Vr.
zet Aur Range of light variation strongly depends on lambda:
zet Aur 4.98 - 5.53 B, 5.36 - 7.33 U. d = 0.039P var:
zet Aur 37.58d <= d <= 38.07d [5486]. Light fluctuations of
zet Aur K star by 0.05m [5539].
tet Aur VB A (B 7.5m, 2", 8, 331deg, 1924).
tet Aur According to [4034] the period of magnetic field variation
tet Aur is 3.618d.
U Boo Delta(m) var (from 0.9m to 2.4m).
V Boo P var. Amplitude strongly varies.
W Boo According to [6994], P = 30d +-.
Z Boo H2O maser.
RS Boo Delta(S) = 2. P var. Before JD2435000 Max =
RS Boo 2418115.5867 + 0.37733691d*E; since JD2435000 - see
RS Boo Table. Changes of the height of maxima: Max (minimal
RS Boo height) = JD2442500 + 533d*E; a shorter cycle of changes
RS Boo 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).
ST Boo Mean elements 1911 - 1974 - see Table. Blazhko effect: Min
ST Boo (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
SW Boo Max = 2421840.295 + 0.5134948d*E [2008, 2011]. Since
SW Boo 1960 - see Table. Secondary oscillation: Max (height of
SW Boo Max) = 2441037.33 + 12.997d*E. According to [4833], the
SW Boo magnitude 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.
TV Boo Blazhko effect, Pi = 16.14d [7116].
TW Boo B - V: +0.11, +0.40. Delta(S) = 12. P var. Before
TW Boo JD2426890 Max = 2420340.551 + 0.53227557d*E;
TW Boo 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
TZ Boo vary from 10.8 to 11.0 V with P ~3.5 yrs; sometimes Min II
TZ Boo is deeper than Min I. Some other parameters of the shape
TZ Boo of light curve are also variable. In ~1960 the period
TZ Boo changed abruptly; other period variations were also noted.
UU Boo B - V: +0.03, +0.44. P var. Period change ~JD2432700
UU Boo [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
UY Boo Max = 2411459.819 + 0.6508552d*E; Max =
UY Boo 2425688.836 + 0.6507849d*E (JD2425500 - 28670) [1702];
UY Boo Max = 2432306.759 + 0.650799d*E (JD2428670 - 32300)
UY Boo [2431]. Since JD2435900 - see Table.
VW Boo Min II 10.93. P var. Nonlinear term:
VW Boo -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
YZ Boo varies [8186].
ZZ Boo Min II 7.44. Possible radio source.
AC Boo Min II 10.55. P var? Depth of minima and level of maxima
AC Boo 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 period is given.
AR Boo Min II 14.5. P var.
AS Boo Blazhko effect is possible.
BD Boo Blazhko effect is possible.
BE Boo Scatter in the light curve near max light;
BE Boo P var? [5264]. The value of the period in the
BE Boo 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.
BL Boo "Anomalous cepheid". Radial velocity cluster member.
BN Boo In the region of the cluster NGC 5466.
BO Boo The shape of the light curve varies: magnitude in
BO Boo Max - from 14.5 to 15.0.
BP Boo 5.51 V.
BR Boo The mean light curve shows scatter which may evidence for
BR Boo the necessity to improve the period.
BU Boo P var. Mean period is given. AO Boo. The mean light curve
BU Boo could not be obtained.
BW Boo Min II 7.17. Min II - Min I = 0.450P. DII = 0.06P. SB1.
BX Boo VB A (B 10.6m, 36", 156deg). P var. According to other
BX Boo sources: Min = 244076730 + 0.741285d*E [7955];
BX Boo Min = 2440767.26 + 0.6080722d*E [5054].
CC Boo The star is not red.
CD Boo The star is not red.
CK Boo Min II 9.23.
CP Boo P > 0.125d.
EL Boo Type E: is also possible.
gam Boo VB A (B 12.5m, 33", 111deg, 1925). Delta(m) var. Radial
gam Boo velocity varies with P = 0.25d +-0.02d [4914].
kap 2 Boo ADS 9173 A (B = kappa1 Boo, 6.69m, SB, F2V, 13",236deg).
kap 2 Boo According to [7015], P = 0.0668d.
kap 2 Boo Beat period ~16d [6086, 7015].
ksi Boo ADS 9413 AB (4.7m, G8V; 6.6m, K4V; A = 4.884", P = 149.95a).
ksi Boo LiI lambda 6708 line is present in the G8V spectrum. Both
ksi Boo spectra show manifestations of chromospheric activity,
ksi Boo emissions of H and K Ca II. Soft X-ray source. Probably it
ksi Boo is component A that is variable, though variability of H
ksi Boo and K CaII emission with the cycle 10 - 11 years
ksi Boo is observed for component B.
i Boo ADS 9494 B (A 5.1m, G0; a = 3.8", e = 0.43, P =
i Boo 225a). Min II 6.29. P var. Min = 2434132.517 +
i Boo 0.267812271d*E + 0.115242d*10**(-9)*E**2 (1916 -
i Boo 1958) [3239]; Min = 2438513.4166 + 0.2678143d*E
i Boo (1947 - 1967) [8191]; since 1968 - see Table. Detailed
i Boo studies of period changes [5222, 7352, 7353, 8181]. Sudden
i Boo period changes at JD2423800, 29300, 32300, 35150 are
i Boo possible. The shape of the light curve and the depth of
i Boo Min II are also variable. According to [2020], it is also
i Boo possible that ADS 9494 A is variable, with the amplitude
i Boo up to 0.09m.
S Cae = +0.33. P < 1d.
X Cae (k - b)2 = 0.22.
RX Cae Variability type and spectral type (F3/F5II) do not agree.
R Cam S2/5:e. P var.
T Cam S5/5e.
U Cam Interfering P1 = 435.45d, P2 = 223.17d; P3 = 3000d [1053].
V Cam H2O, SiO maser.
Y Cam EA/SD. SB1. Min II 10.60. P var. Min =
Y Cam 2424434.5071 + 3.3054975d*E + 0.1215d*
Y Cam sin (0.0543deg*E + 186.8deg) (JD2411400 - 33300) [0978];
Y Cam Min = 2437375.4923 + 3.3055069d*E + 5.3d*10**(-8)*E**2
Y Cam (JD2437375 - 41000) [7166]; since JD2440000 - see Table.
Y Cam The primary component is a DSCTC variable [7166] with
Y Cam A <= 0.05m B. According to [4192], the pulsational period
Y Cam is possibly synchronized with the orbital motion and
Y Cam remains practically constant (0.066458d) during a long time
Y Cam interval.
Z Cam SB2. Lower conjunction of the G component
Z Cam T = 2438470.841 + 0.289840d*E [5365]. Outside outbursts
Z Cam the light curve is modulated with spectroscopic elements
Z Cam and has a shoulder at the phase 0.88P and a broad, shallow
Z Cam dip at the phase 0.15P. Outside maxima flickering up to
Z Cam 0.5m with P ~ 16s - 18s is observed. During maxima
Z Cam brightness 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 -
RU Cam 1917), Min = 2421315.3 + 22.121d*E (1917 - 1922),
RU Cam Min = 2423195.6 + 22.217d*E (1922 - 1931), Min =
RU Cam 2426350.4 + 22.138d*E (1931 - 1951), Min =
RU Cam 2433700.2 + 22.162d*E (1951 - 1961), Min =
RU Cam 2437356.9 + 22.055d*E (1961 - 1965) [3243].
RU Cam Unusual variable. The shape of the light curve varies.
RU Cam Before 1964 broad maxima and sharp minima were observed;
RU Cam Delta(m) varied by the factor of 2, with a possible cycle
RU Cam 5.1a [3241]. After 1964 - 1966 Delta(m) decreased abruptly
RU Cam (to 0.4m - 0.1m and smaller), the light curve became
RU Cam symmetric; the mean light varies in the range of 0.3m B.
RU Cam The period varies irregularly in the interval
RU Cam 19.4d - 23.5d. Groups of oscillations are observed to
RU Cam replace one another, with phase shifts up to 0.5p [4206].
RU Cam 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:
SS Cam +2.04d*10**(-9)*E**2.
SV Cam Depth of Min II 0.15m: pg. P var. A cycle of 50a may be
SV Cam present in period changes. The elements in the Table are
SV Cam valid since 1967.5.
SW Cam P var. Before JD2437600 Max = 2434448 + 254.2d*E. Since
SW Cam JD2440000 - see Table.
SZ Cam Member of the open cluster NGC 1502. ADS 2984 B (A = NSV
SZ Cam 1458 7.1m V; B 18", 304deg). Min II 7.24, D II = 0.17P.
SZ Cam P var. Since 1970 - see Table; earlier
SZ Cam 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];
UZ Cam since JD2440000 - see Table.
WW Cam d = 0.013d. Min II 11.1.
XX Cam During 1898 - 1980 a single symmetric Min JD2429632 was
XX Cam observed which lasted for 94d. Brightness fluctuations up
XX Cam to 0.2m during several dozens of minutes [4271]. Hydrogen
XX Cam deficiency and carbon excess in the spectrum. Some authors
XX Cam express doubt about the star's being an RCB variable; in
XX Cam 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 +
AH Cam 0.3687404d*E (JD2427000 - 33897) [2305]. Since
AH Cam JD2438000 - see Table. Magnitude in Max varies with a
AH Cam possible cycle Pi = 46 P [3506].
AK Cam P var. Min = 2426393.180 + 2.226780d*E (JD2426390 - 36610)
AK Cam [2594]; since JD2436000 - see Table.
AS Cam d = 0.009P. Min II 8.97, DII = 0.06P, Min II - Min I =
AS Cam 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 Detailed spectral studies [7191], [7192].
AY Cam Min II 10.23, DII = 0.12P, dII = 0.02P. According to
AY Cam [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
BK Cam were observed which came to an end by 1937 [4282].
BM Cam SB1 (P = 80.174469d; e = 0.35). Epoch of Min light is given.
CZ Cam P = 267.79d, semiregular behavior unusual for B5 stars.
R Cnc SiO maser.
S Cnc In the field of Praesere (NGC 2632) cluster. d = 0.015P.
S Cnc Min II 8.39. P var.
U Cnc VB A (B 3"). In the field of Praesepe (NGC 2632) cluster.
V Cnc S0.5/6e. 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],
RW Cnc Max = 2421339.380 + 0.5471932d*E +
RW Cnc 0.57d*10**(-9)*(E - 5800)**2 + 0.028d*cos0.0215deg*
RW Cnc (E + 2260) + f(psi, hi); here the last term is the sum of
RW Cnc two short period oscillations and is given in graphical
RW Cnc form, since the main period (0.547d) varies with
RW Cnc Pi1 = 29.9d and Pi2 = 91.1d. Magnitude in Max varies from
RW Cnc 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),
RY Cnc non-member. B - V: +0.58, +1.05. P var. Before JD2436000
RY Cnc Min = 2429334.445 + 1.0929500d*E; since
RY Cnc 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
SY Cnc [4286].
TT Cnc (k - b)2 = 0.11. P var. Before JD2430700
TT Cnc Max = JD2425647.452 + 0.5634445d*E [3506].
TT Cnc Since JD2439800 - see Table. Blazhko effect, Pi = 89d
TT Cnc [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
TX Cnc 10.32.
TY Cnc d = 0.013P. P var.
UU Cnc Min II 9.2, JD (Min II) 2435608.5. SB1. The light curve is
UU Cnc unstable. 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
VZ Cnc observed. According to [2125], for the middle of
VZ Cnc the ascending branch T () = 2433631.84615 +
VZ Cnc 0.17836376d*E + 0.00193d*sin(2*pi*psi() -
VZ Cnc 0.00371d*cos*2*pi*psi(); here the phase of the beat
VZ Cnc period psi() is computed with the elements T() =
VZ Cnc Spectral investigation [2126].
WW Cnc According to [7531], the period does not vary since 1933.
WW Cnc A number of minima by
WW Cnc 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 In the region of the Praesepe (NGC 2632) cluster.
XZ Cnc Min II 10.2.
YY Cnc According to [3263], the star is probably an irregular
YY Cnc variable.
YZ Cnc Oscillations with P = 133.2m are observed in maximum light
YZ Cnc [6249].
ZZ Cnc d = 0.02P:.
AC Cnc Min II 14.7. = 14.5.
AC Cnc The brightness outsibe eclipses varies in the range 13.8 -
AC Cnc 15.2B. 3 deep minima contradict the tabulated
AC Cnc elements [4460]. The identification with the X-ray
AC Cnc 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.
AH Cnc Nonlinear term: +1.56d*10**(-10)*E**2.
AH Cnc Cyclic period variations (with different cycles) are also
AH Cnc possible [4475].
AO Cnc Min II 13.4.
AP Cnc P var?
AU Cnc Possible member of the cluster praesepe (NGC 2632).
AV Cnc Possible member of the cluster Praesepe (NGC 2632).
AW Cnc Possible member of the cluster Praesepe (NGC 2632).
AX Cnc Possible member of the cluster Praesepe (NGC 2632).
AY Cnc Possible member of the cluster Praesepe (NGC 2632).
AZ Cnc Possible member of the cluster Praesepe (NGC 2632).
BB Cnc Delta(mu) > 6.0. Possible member of the cluster
BB Cnc Praesepe (NGC 2632).
BC Cnc Delta(mu) > 4.0. Possible member of the cluster
BC Cnc Praesepe (NGC 2632).
BD Cnc Possible member of the cluster Praesepe (NGC 2632).
BE Cnc Possible member of the cluster Praesepe (NGC 2632).
BG Cnc Possible member of the cluster Praesepe (NGC 2632).
BH Cnc Possible member of the cluster Praesepe (NGC 2632).
BI Cnc The elements were determined by Winzer. Epoch of Max
BI Cnc in U band is given.
BK Cnc Possible member of the cluster Praesepe (NGC 2632).
BM Cnc SB (P = 585.4154d [6568]). The elements in the Table
BM Cnc represent the moments of maximal (B - V).
BN Cnc Member of the cluster Praesepe (NGC 2632).
BQ Cnc SB.Member of the cluster Praesepe (NGC 2632).
BR Cnc VB A (B 14.2m, 30", 268deg). Member of the cluster
BR Cnc Praesepe (NGC 2632).
BS Cnc Member of the cluster Praesepe (NGC 2632).
BT Cnc Member of the cluster Praesepe (NGC 2632).
BT Cnc Oscillations with other periods are superimposed.
BU Cnc Member of the cluster Praesepe (NGC 2632). According to
BU Cnc [4483], P = 0.071d is not confirmed; during different
BU Cnc nights P = 0.0534d, P = 0.059d and several other
BU Cnc periodicities were observed.
BV Cnc Member of the cluster Praesepe (NGC 2632).
BW Cnc Member of the cluster Praesepe (NGC 2632).
BX Cnc Member of the cluster Praesepe (NGC 2632).
BY Cnc Member of the cluster Praesepe (NGC 2632).
BZ Cnc In the region of the Praesepe (NGC 2632) cluster.
CC Cnc Cycle <= 90d.
CD Cnc Possible member of the cluster Praesepe (NGC 2632).
CE Cnc In the region of the Praesepe (NGC 2632) cluster.
CF Cnc In the region of the Praesepe (NGC 2632) cluster.
CG Cnc In the region of the Praesepe (NGC 2632) cluster.
CH Cnc In the region of the Praesepe (NGC 2632) cluster.
CI Cnc Possible member of the cluster Praesepe (NGC 2632).
CK Cnc In the region of the Praesepe (NGC 2632) cluster.
CL Cnc In the region of the Praesepe (NGC 2632) cluster.
CM Cnc Possible member of the cluster Praesepe (NGC 2632).
CN Cnc Possible member of the cluster Praesepe (NGC 2632).
CO Cnc In the region of the Praesepe (NGC 2632) cluster.
CP Cnc In the region of the Praesepe (NGC 2632) cluster.
CR Cnc In the region of the Praesepe (NGC 2632) cluster.
CS Cnc In the region of the Praesepe (NGC 2632) cluster.
CU Cnc G 9-8 = G 40-25. VB A (B = CV Cnc, 13", 347deg),
CU Cnc common mu. In the region of Praesepe (NGC 2632) cluster,
CU Cnc non-member.
CV Cnc G 40-26. VB B (A = CU Cnc).
CY Cnc Member of the cluster Praesepe (NGC 2632).
CZ Cnc Equinox in [8354] must be 2000.0.
DD Cnc In the region of the Praesepe (NGC 2632) cluster.
DF Cnc In the region of the Praesepe (NGC 2632) cluster.
DF Cnc Posibly non-member.
DG Cnc In the region of the Praesepe (NGC 2632) cluster.
DG Cnc Possibly non-member.
DH Cnc Possible member of the cluster Praesepe (NGC 2632).
DI Cnc Possible member of the cluster Praesepe (NGC 2632).
DL Cnc VB. In the region of the Praesepe (NGC 2632) cluster.
DM Cnc Possible member of the cluster Praesepe (NGC 2632).
DN Cnc In the region of the Praesepe (NGC 2632) cluster.
DO Cnc In the region of the Praesepe (NGC 2632) cluster.
DP Cnc In the region of the Praesepe (NGC 2632) cluster.
DQ Cnc In the region of the Praesepe (NGC 2632) cluster.
DQ Cnc Possibly non-member.
DR Cnc In the region of the Praesepe (NGC 2632) cluster.
DS Cnc In the regiom of the Praesepe (NGC 2632) cluster.
DS Cnc Possibly non-member.
DT Cnc In the region of the Praesepe (NGC 2632) cluster.
DU Cnc In the region of the Praesepe (NGC 2632) cluster.
FV Cnc The type is doubtful.
kap Cnc SB (P = 6.39316d). In [4487] the light variability was not
kap Cnc confirmed.
R CVn P var. Max = 2411768 + 325.4d*E (JD2411730 - 26430) [1701];
R CVn Max = 2432074 + 332.8d*E
R CVn (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.
W CVn 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 +
Z CVn 0.6538236d*E (JD2413000 - 23170); Max =
Z CVn 2423860.355 + 0.6539052d*E (JD2423860 -
Z CVn 31800) [1702]; Max = 2432943.645 + 0.653824d*E
Z CVn (JD2431800 - 40200) [6457]. Since JD2438900 - see Table.
Z CVn Blazhko effect: Min. ampl. = 2439176.12 + 22.75d*E [3267].
Z CVn Amplitude varies by 0.5m B, extremal periodic deviations
Z CVn of the epoch of Max from linear elements are +-0.02d.
Z CVn Delta(S) = 8.
RR CVn B - V: +0.09, +0.45. [Fe/H] = -1.33.
RR CVn The light curve shape and Delta(m) var.
RS CVn Min II 8.19; Min II - Min I = 0.506P; d = 0.033P.
RS CVn P var. Nonlinear term: -1.00d*10**(-8)*E**2. Wave-like
RS CVn distorsion with the amplitude from 0.09m up to 0.20m and
RS CVn with the period 4.7917d close to the orbital one is
RS CVn observed on the light curve out of eclipses [7209].
RS CVn The wave is migrating on phase in the direction of phase
RS CVn decreasing with a migration period of 9.48 years [5800].
RU CVn B - V: +0.10, +0.39. P var. Max = 2420227.338 +
RU CVn 0.5732502d*E (JD2418801 - 29436) [5436]; Max =
RU CVn 2420227.398 + 0.57324647d*E (JD2418979 -
RU CVn 36665) [3271]; since JD2434483 - see Table.
RV CVn V141 (M3/NGC 5272). Not a member of the cluster.
RV CVn 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 +
RZ CVn 0.56740036d*E (JD2424620 - 31000) [0188];
RZ CVn Max = 2437823.433 + 0.5674174d*E (JD2434470 -
RZ CVn 37830); since JD2438200 - see Table.
ST CVn P var? Delta(S) = 4.8.
SV CVn P var. Max = 2427434.911 + 0.66805653d*E
SV CVn (JD2426000 - 32000) [0752]; since JD2439500 - see Table.
SW CVn P var. Max = 2431139.791 + 0.44164922d*E
SW CVn (JD2425640 - 32000) [0752]; since JD2436200 - see Table.
TX CVn SB2 (P = 70.8d) [4504].
UU CVn In the region of the globular cluster NGC 5466. P var.
UU CVn Max = 2437817.312 + 0.5409589d*E (JD2436360 - 39945);
UU CVn since JD2439945 - see Table.
UV CVn In the region of globular cluster NGC 5466, non-member.
UV CVn P var. Max = 2419446.156 + 0.6316090d*E (JD2419440 - 34455);
UV CVn 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
VW CVn (JD2427900 - 36000); since JD2435900 - see Table. The
VW CVn variable is not marked on the map. It is by 6mm to the
VW CVn 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? Blazhko effect
WY CVn is possible.
WZ CVn V 206 (M3/NGC 5272). Non-member? Blazhko effect.
XX CVn In the region of M3 (NGC 5272) globular cluster. Member
XX CVn 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,
AI CVn 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
AM CVn disappears. The depth of Min I changes also. Epoch of
AM CVn Min I is given in the Table. P var; dP/dt = +0.012s per
AM CVn year. Elements for 1978 are given in the Table. The
AM CVn brightness fluctuates with the cycle of 115 - 120s,
AM CVn sometimes the periodicity with P = 26.3s is observed.
AM CVn Probably it is a close binary semidetached system of two
AM CVn 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.
AQ CVn A flare lasting 20 minutes was observed.
BF CVn G 123-75 = G 164-32. VB A (B = G 164-31, 13.16m,
BF CVn dM3.5e; 17", 225deg). Flares in the combined light of the
BF CVn 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?
CS CVn HIPPARCOS data contradict the luminosity class V.
alf 2 CVn VB A (B 5.60m, F0V, 19.6", 228deg).
alf 2 CVn Epoch of Min is given.
R CMa Min II 5.78. P var [3280, 6314].
R CMa 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
Z CMa profiles. The star is located in a nebula rich in details.
Z CMa A bright wisp of nebulosity near the star has continuons
Z CMa spectrum, probably identical to that of the star [4002].
RR CMa Min II 13.1.
RT CMa Min II 11.5.
RT CMa P = 1.293745d is possible taking into account the epoch
RT CMa from [3283].
RX CMa d = 0.027P. Min II 11.1. P var. During JD2441700 - 43000
RX CMa - see Table.
RZ CMa P var? Since JD2435500 - see Table.
SW CMa Min II 9.9. Min II = JD2426709.366; Min II - Min I =
SW CMa 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.
UW CMa Minima are asymmetric; other peculiarities of the light
UW CMa are observed. A number of spectral lines have P Cyg
UW CMa profiles.
UW CMa The line profiles are observed to vary with the phase of
UW CMa the orbital period, and also ([7227], according to Sanyal)
UW CMa 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,
VY CMa D 11m, 2.9", 347deg, ...). H2O, OH, SiO maser.
VY CMa B - V: +2.3.
VY CMa In the region of the
VY CMa young open cluster NGC 2362. Embedded in a
VY CMa reflecting nebula. The companions may be details
VY CMa of the nebula; some of them are probably variable [2159,
VY CMa 3287]. Surrounded by an envelope of gas and dust or a disk
VY CMa of 0.45" (lambda = 5 mkm) angular size. Secular decrease
VY CMa of brightness since 1801. Cyclic variations of brightness
VY CMa with Delta(m) from several tenths of a magnitude to 3m on
VY CMa time scale from 200d to 1900d. TiO and ScO emission bands
VY CMa in the spectrum. Spectroscopic studies [3287, 5282, 6133].
WW CMa RR, Max = 2428570.09 + 0.499355d*E [0613]. CEP,
WW CMa Max = 2428146.6 + 5.7660d*E [0514]. These systems of
WW CMa elements are contradicted by 94 photographic observations
WW CMa (Erleksova) and 12 photoelectric observations (Irwin,
WW CMa [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. SB2.
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).
EW CMa SB (P = 0.261975d). Brightness variations are not related
EW CMa to the orbital phase. Shell star (probably an extended
EW CMa atmosphere of one of the components and the common shell
EW CMa 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 superimposed
EY CMa by secondary ones (P = 0.2033d and 0.1690d); beat effect,
EY CMa Pb ~2.00d [7243].
EZ CMa SB. In the centre of the ring HII region S 308. Member of
EZ CMa the open cluster collinder 121. Epoch of Max light is
EZ CMa given. The companion is probably a neutron star. The shape
EZ CMa of the light curve, Delta(m), phases of maxima and minima
EZ CMa and mean light vary from one observational season to
EZ CMa another.
FF CMa Min II 7.6. Elements should be improved. Member of the
FF CMa 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
FN CMa combined light variation is given in the Table.
FN CMa Associated with the nebula vB 95. According to [6135],
FN CMa 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],
FS CMa [NiII], [CrII], [SII], [OI], FeII. IR excess
FS CMa (1.6 - 20 mkm). P Cyg profiles of Balmer lines vary in the
FS CMa time scale of hours. Brightness varies from night to night
FS CMa by 0.1m and during a night by 0.03m, sometimes in
FS CMa correlation with spectral changes [6636]. Spectral
FS CMa studies [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
FZ CMa CMa OB1.
GG CMa Member of the open cluster Cr 132a.
GU CMa ADS 5713 AB (7.5m, 8.2m, 0.6", 187deg, 1919). SB?
GU CMa In the HII region S 293.
GY CMa According to [8380], does not vary.
GZ CMa SB2.
HK CMa Epoch of Min is given.
HL CMa 1E 0643.0-1648. SB (P ~0.217d); Lx/Lopt var (0.002 - 1).
IU CMa Type LBV: is also possible.
MO CMa The amplitude can have been overestimated (M. Grenon,
MO CMa private communication).
NO CMa Type LBV: is also possible.
bet CMa In 1971 - 72 the observations were described by the
bet CMa combination of the tabulated elements (period P1) and the
bet CMa following systems of elements:
bet CMa Max = 2441296.0705 + 0.251300d*E, (P2);
bet CMa Max = 2441296.032 + 0.23904d*E, (P3);
bet CMa Max = 2441296.065 + 0.12501d*E, (P1/2);
bet CMa Max = 2441296.124 + 0.12565d*E, (P2/2).
bet CMa Beat periods: 49.198d, 5.442d, 4.900d.
bet CMa Since 1908 P1 increases, P2 decreases. 12 overtone and
bet CMa resonance periods were found in [3454].
ksi 1 CMa ADS 5176 A (B 14.5m, 25", 147deg; C 14.0m, 29", 303deg,
ksi 1 CMa 1897).
sig CMa ADS 5719 A (14.2m, 11", 153deg, 1926).
tau CMa SB, Porb = 154.90d.
ome CMa SB?
R CMi SC4/10e.
T CMi P var. Max = 2422456 + 324.2d*E (JD2416610 -
T CMi 22800); Max = 2430896 + 311.2d*E (JD2423090 -
T CMi 30900); since JD2430900 - see Table.
U CMi There is a hump on the ascending branch looking sometimes
U CMi as a secondary maximum. The light curve for 1904 - 1970
U CMi [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 (JD2425234 - 708);
SY CMi 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;
YZ CMi additional term: -0.00003919514d*E*(E + 1)/2. Periodical
YZ CMi light variations with the amplitude 0.12m (11.26 - 11.38 V)
YZ CMi are superimposed by strong flares.
AG CMi P var. Min = 2434698.670 + 1.6645729d*E (JD2426350 -
AG CMi 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 =
AK CMi 2425352.348 + 0.56589534d*E (JD2424880 -
AK CMi 35550) [1728]. Since JD2435600 - see Table.
AL CMi Observations in the interval JD2424880 - 25950 are
AL CMi represented by the elements: Max = 2425243.631 + 0.55050d*E.
AL CMi 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:.
BO CMi Several episodes of outburst-like activity.
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
RV Cap (JD2417400 - 33610) [0323]. Since JD2433850 - see Table.
RV Cap Light curve and period vary with the Blazhko effect
RV Cap period Pi = 225.5d [6464]. Semiamplitude of deviations
RV Cap from linear elements is +-0.032d. 0.14P <= M - m <= 0.25P.
RV Cap (k - b)2 = 0.05.
RW Cap d = 0.020P. Min II 9.9. P var. Min I = 2418924.594 +
RW Cap 3.3923922d*E (JD2418920 - 24000) [6774];
RW Cap Min I = 2424003.014 + 3.3923457d*E (JD2424000 -
RW Cap 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);
TW Cap P = 28.61700115d (JD2417600 - 24000) [1331];
TW Cap Max = 2426211.90 + 28.59497d*E (JD2421400 -
TW Cap 26200) [2390]; Max = 2435664.8 + 28.5578d*E
TW Cap (JD2426210 - 37500) [2309]; since JD2437500 - see Table.
TW Cap 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
TY Cap (JD2425500 - 35000); since JD2435000 - see Table.
UW Cap Min II 11.5; Min II - Min I = 0.5P. P var? Min I =
UW Cap 2434627.290 + 1.399118d*E (JD2427000 - 35000);
UW Cap 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.
BH Cap Type RR: is also possible.
BN Cap The variability may be due to the fainter (B) component.
del Cap VB A (B 15.8m, 69", 94deg; C 12.7m, 119", 302deg,
del Cap 1911); mu = 0.391", P = 138.8deg. Min II 2.90.
del Cap 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 -
U Car 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)
Y Car [5119]. The fundamental mode period P0 is given in the
Y Car Table (A = 0.58m). The first overtone period P1 = 2.55954d
Y Car [5119] (A = 0.28m). P1/P0 = 0.7032.
RR Car P var.
= 154d (JD2421500 - 23500);
= 259d
RR Car (JD2426400 - 30100);
= 154d (JD2430400 - 33100).
RR Car S6.5/1- .
RT Car In the region of the cluster Tr 15.
RY Car There is a close companion 14.3 pg. P var.
RY Car Max = 2418475 + 416d*E (JD2415140 - 18500);
RY Car Max = 2429901 + 417.3d*E (JD2423600 - 32900);
RY Car 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 amplitude of
TZ Car the short cycle is large in mean brightness maximum and
TZ Car 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]
VV Car (10h 36.0m -58deg 56', 1950.0) embedded in a nebula.
VY Car VB A (B 11.07m; B 9V:, 10", 150deg). P var.
VY Car Nonlinear term: -0.000021d*E**2 (JD2410000 - 44200).
VY Car The latest observations may be represented also by linear
VY Car elements: Max = 2444161.16 + 18.9138d*E
VY Car (JD2441000 - 44200). [A/H] = 0.4.
WZ Car P var. Max = 2419981.099 + 23.000945d*E (JD2410000 - 20000)
WZ Car [0025]; Max = 2423984.12 + 23.0054d*E (JD2419800 - 25500)
WZ Car [0322]; Max = 2434914.86 + 23.0075d*E + 0.000025d*E**2
WZ Car (JD2434500 - 41200) [2309]; since JD2434500 - see also
WZ Car Table.
XX Car P var. Max = 2420769.703 + 15.723704d*E (JD2410000 - 22500)
XX Car [0025]; P = 15.7196d (JD2423000 - 30000) [0003]; since
XX Car JD2434500 - see Table; elements given in the Table contain
XX Car a nonlinear 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
AF Car JD2435000 - see Table.
AG Car Central star of the low-excitation planetary nebula
AG Car P.K.289-0.1 ejected probably during a nova-like outburst
AG Car of the star about 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). In the region of
BO Car the cluster Tr 15. Cluster non-member.
BP Car P = 4.82246d?
BS Car In the region of the cluster 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 In 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
DH Car (Min brightness).
DI Car Besides Cepheid-like light variations with the amplitude
DI Car 1.7m and elements Max = 2438553.70 + 29.210d*E
DI Car (JD2438465 - 40300) [5324] large weakenings of brightness
DI Car 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 In the region of the cluster NGC 3532.
EH Car VB A (B 15", 320deg).
EK Car In the region of the cluster NGC 3532.
EM Car Min II 8.9.
EN Car In the region of the cluster Tr 18.
EQ Car d = 0.030P. Min II 13.7.
ER Car In the region of the cluster NGC 3532.
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 (JD2423790 - 35300)
FI Car [0046, 2309]. Since JD2435300 - see Table.
FK Car VB.
FO Car VB A (B 14m, 7", 90deg). P var. Max = 2434922.531 +
FO Car 10.3559d*E (JD2423700 - 35300) [6006]; since JD2436000
FO Car - see Table. B - V: +1.13, +1.43.
FP Car d = 0.01P:.
FQ Car In the region of the cluster Tr 18.
FS Car In the region of the very poor cluster N 99 [7374] (10h
FS Car 36.0m -58deg 56', 1950.0) embedded in a nebula. Min II
FS Car 10.9.
FT Car According to [2197] spectrum C. Misidentification is
FT Car possible.
FV Car VB A (B 13m, 10", 135deg). P var. There are two additional
FV Car terms in the elements given in the Table:
FV Car -0.1065d*10**(-7)*E**2 - 0.584d*10**(-11)*E**3.
FV Car d = 0.02P:. Min II 13.0.
GG Car Min II 9.5. Gas and dust envelope.
GH Car In the region of the cluster Tr 18.
GK Car In the region of the cluster Tr 19. Min II 13.2.
GL Car In the region of the cluster NGC 3572. Min II 10.31.
GL Car System with the apsidal motion; e = 0.157, omega = 99deg.
GL Car There are sinusoidal terms in the elements for Min I given
GL Car in the Table: +0.121d sin(0.094389deg*E) -
GL Car 0.007d sin(0.188778deg*E);
GL Car Min II = 2424263.236 + 2.4222338d*E -
GL Car 0.121d sin(0.094389deg*E) - 0.007d sin(0.188778deg*E).
GL Car DII = 0.17P.
GM Car In the region of the very poor cluster N 99 [7374] (10h
GM Car 36.0m -58deg 56', 1950.0) embedded in a nebula.
GM 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 oscillation with
GZ Car an amplitude 0.16m are given in the Table. For the first
GZ Car overtone oscillation with an amplitude 0.07m
GZ Car Max = 2440742.4 + 2.93424d*E. Epochs of maxima and
GZ Car amplitudes are given according to [5175].
HH Car VB A (B 13.0m, 5", 260deg; C 11.11m, 13", 337deg; D 12.65m,
HH Car 15", 7deg). d = 0.02P. Min II 10.66. P var [8094].
HH Car Min I hel = 2430860.162 + 3.2315393d*E (JD2427590 - 35260)
HH Car [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
HK Car 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
HP Car 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 In the region of the cluster NGC 2602.
IL Car Min II 14.4.
IN Car It is possible that the period must be doubled.
IQ Car In the region of the cluster NGC 3532.
IR Car In the region of the cluster NGC 3532. 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
IW Car amplitude of main oscillations - from 1.3m to 0.3m.
IX Car In the centre of a bright nebula with the diameter 2.4'.
IZ Car Declination in [0085] is wrong by 3deg. Identical to
IZ Car V336 Car, see [6316].
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:
OY Car Min I hel = 2443993.553241 + 0.0631209247d*E [5185];
OY Car D = 0.050P, d = 0.044P. The hump on the light curve is
OY Car observed at the phase of 0.75P. Depth of Min I varies
OY Car 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). Flickering resembles V818 Sco.
QU Car Variations by 0.2m in 90s were observed. No periodicity
QU Car was found. Emission lines He II 4686, CIV - NIII 4630 -
QU Car 4650 and sometimes weak hydrogen absoptions (corresponding
QU Car to A or B type) are noticeable in the spectrum [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
QZ Car Collinder 228. Min II 6.43. Two SB1 systems (A and B),
QZ Car B is eclipsing (A: SB1, P = 20.73d, O9.5 I,
QZ Car Delta(m) = 0.6m). Combined brightness is given.
V0341 Car In the variable reflecting nebula IC 2220. In the region
V0341 Car of the open cluster NGC 2516. IR excess.
V0343 Car VB. SB (P = 133.92d).
V0347 Car Deep Min II.
V0348 Car In the open cluster IC 2581. Min II 8.9.
V0354 Car Very red.
V0356 Car Member of the cluster NGC 2516.
V0357 Car SB (P = 6.74483d [4627]).
V0361 Car In the region of the cluster NGC 3293.
V0365 Car In the region of the cluster NGC 3532.
V0367 Car Min II 7.54.
V0373 Car Member of the cluster NGC 2516.
V0374 Car Member of the cluster NGC 2516.
V0375 Car P = 0.264d or 0.359d.
V0376 Car VB A (B 6.83m, B 9.5V, 41", 75deg).
V0378 Car In the open cluster NGC 3293.
V0379 Car In the open cluster NGC 3293.
V0380 Car In the open cluster NGC 3293.
V0381 Car In the open cluster NGC 3293.
V0382 Car In the region of the cluster NGC 3532.
V0385 Car Depth of Min II 0.04m. Surrounded by a ring nebula RCW 58.
V0491 Car Mean magnitude 9.69.
V0493 Car SB, Porb = 3.368d.
V0498 Car Type BE: is also possible.
V0534 Car Flare-like activity.
eta Car In the emission nebula NGC 3372 in the region of the
eta Car cluster Tr 16. A very massive young star surrounded by an
eta Car expanding gas and dust shell with the diameter 2" at 2mu
eta Car and 6.5" at 12.2mu. Maximum brightness was observed in
eta Car 1843. Since 1880 varies in the range 5.9 - 7.9 V. In the
eta Car interval JD2434000 - 41000 Max = 2434037 + 1110d*E. There
eta Car are emission lines of H, HeI, FeII, [FeII], etc. in the
eta Car spectrum. Description of the spectrum [5251, 7279].
eta Car Soft X-ray source of variable intensity.
khi Car Soft X-ray source.
R Cas VB A (B 14.5m, 14", 273deg). SiO, OH maser;
R Cas sometimes H2O emission.
T Cas SiO maser. ZrO bands in the infrared spectral region.
U Cas S4.5/4e.
W Cas SC5/9e.
X Cas P var: Max = 2426650 + 432.32d*E (JD2416750 - 27060);
X Cas Max = 2432870 + 413.6d*E (JD2427060 - 32870);
X Cas Max = 2437948 + 423.0d*E (JD2432870 - 39210).
X Cas 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)
RS Cas [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).
RW Cas Since JD2430000 - see Table. [A/H] = 0.3.
RX Cas Unigue rapidly evolving eclipsing system. 9.12<=Min II<=9.49;
RX Cas Min II - Min I = 0.5070P. P var. Nonlinear term:
RX Cas +1.017d*10**(-5)*E**2. Observations may be represented
RX Cas also by three systems of elements: Min I =
RX Cas 2416250.889 + 32.31481d*E (0 <= E <= 286,
RX Cas JD2416250 - 25482); Min I = 2416248.835 + 32.32145d*E
RX Cas (331 <= E <= 554, JD2426940 - 34155);
RX Cas Min I = 2416244.990 + 32.32765d*E (734 <= E <= 876,
RX Cas JD2439970 - 44570). Brightness of the system out of
RX Cas eclipses periodically varies within 8.6m - 9.0m with
RX Cas elements Max = 2416198 + 516.06d*E [5036]. Max - Min =
RX Cas 233d = 0.45P [0881]. Strong emissions of H, NV, CIV,
RX Cas SIIV, FeIII. Powerful gaseous stream and accretion
RX Cas phenomena are possible.
RY Cas [A/H] = 0.0.
RZ Cas Min II 6.26. The light curve shape var; d var
RZ Cas (0.000P <= d <= 0.009P). P var, variations are irregular.
RZ Cas Mean elements based on visual and photographic
RZ Cas observations: Min I = 2416886.8806 + 1.195253065d*E
RZ Cas (JD2416800 - 26700) [8820], Min I = 2432820.7853 +
RZ Cas 1.1952517d*E (JD2426700 - 34000) [0938]. From
RZ Cas photoelectric observations: Min I = 2432115.5827 +
RZ Cas 1.1952472d*E (JD2429870 - 30400); Min I =
RZ Cas 2432085.7011 + 1.195259d*E (JD2432000 - 32460);
RZ Cas Min I = 2434349.5130 + 1.1952525d*E (JD2432450 - 34420);
RZ Cas Min I = 2434703.3035 + 1.195238d*E (JD2434420 - 34705);
RZ Cas Min I = 2435934.4087 + 1.1952499d*E (JD2434705 - 35950);
RZ Cas Min I = 2438829.2818 + 1.195243d*E (JD2436800 - 39100);
RZ Cas Min I = 2440182.3089 + 1.195259d*E (JD2439380 - 40200);
RZ Cas Min I = 2441333.3257 + 1.195244d*E (JD2440500 - 41350);
RZ Cas Min I = 2442327.7798 + 1.1952521d*E (JD2441550 - 42350);
RZ Cas since JD2442850 - see Table.
SU Cas [A/H] = -0.1.
SV Cas P var. Max = 2421839 + 279.3d*E (JD2417600 -
SV Cas 21900); Max = 2430450 + 281.7d*E (JD2422500 -
SV Cas 31900); since JD2432600 - see Table.
SX Cas VB A (B 11.5m, 19", 250deg, 1966). Min II 9.32. The light
SX Cas curve shape var. DII = 0.171P:, dI = 0.036P, dII = 0.050P.
SX Cas P var. Min I = 2433963.267 + 36.56727d*E (JD2418000 -
SX Cas 37000); since JD2438700 - see Table. Strong emissions
SX Cas of H, NV, CIV, SIIV, FeIII. Gaseous streams and accretion
SX Cas phenomena.
SY Cas VB? P var. Max = 2417911.547 + 4.070969d*E
SY Cas (JD2417000 - 34000); since JD2434000 - see Table.
SZ Cas P var. Max = 2421261.66 + 13.6009d*E (JD2416700 - 21260);
SZ Cas Max = 2426650.20 + 13.6072d*E (JD2421260 - 27170) [8821];
SZ Cas Max = 2429727.240 + 13.61744d*E (JD2427170 - 33050);
SZ Cas Max = 2436810.92 + 13.62655d*E (JD2433050 - 38720);
SZ Cas since JD2438720 - see Table. [A/H] = -0.6.
TU Cas Fundamental mode period P0 is given in the Table; the
TU Cas corresponding amplitude is 0.69m. First-overtone period
TU Cas P1 = 1.51830d; the corresponding mean amplitude decreased
TU Cas from 0.4m to 0.25m during 67 years [5078]. P1/P0 = 0.71.
TU Cas M - m var (0.17P <= M - m <= 0.35P).
TV Cas d = 0.01P. Min II 7.34. The light curve shape var.
TV Cas Period of these variations - 600d [8822]. P var. Mean
TV Cas elements based on visual and photographic observations:
TV Cas Min I = 2432827.7665 + 1.81260983d*E (JD2415650 - 32800)
TV Cas [1926]. From photoelectric observations Min I =
TV Cas 2432827.7665 + 1.8126142d*E (JD2432800 - 36490);
TV Cas Min I = 2436483.8091 + 1.81255d*E (JD2436480 - 36980);
TV Cas Min I = 2438472.2386 + 1.81263d*E (JD2437000 - 38500);
TV Cas Min I = 2438829.3230 + 1.8126048d*E (JD2438470 - 41750);
TV Cas 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);
TY Cas Max = 2428965 + 623.8d*E (JD2427000 - 41500);
TY Cas 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 (JD2417000 - 32500);
VV Cas since JD2432500 - see Table. [A/H] = -0.2.
VW Cas [A/H] = 0.0.
WY Cas In the region of the cluster NGC 7789.
WY Cas The spectrum of the G type star is seen in minimum light
WY Cas [3502]. The existence of a physical companion is possible.
WY Cas S6/6-e.
WZ Cas VB A (optical companion B 8.7m, 58", 89deg). SC7/10e.
WZ Cas Light variations are sometimes taking place with doubled
WZ Cas 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 +
AB Cas 1.366863d*E (JD2425400 - 33150); Min I =
AB Cas 2433616.532 + 1.366876d*E (JD2433150 - 37000);
AB Cas Min I = 2440475.5216 + 1.3668783d*E (JD2437000 -
AB Cas 41600); since JD2441600 - see Table.
AB Cas The A3 component is a DSCT type variable with the elements:
AB Cas Max hel = 2444912.1759 + 0.0582874d*E [8825]; amplitude
AB Cas 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 curve 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;
AR Cas D 9.8m, 76", 268deg; E 11.28m, 43", 115deg; F 11.06m, 69",
AR Cas 338deg; G 11.11m, 67", 348deg). Min II 4.86;
AR Cas Min II - Min I = 0.614P; DII = 0.076P; dII = 0.037P.
AS Cas VB A (B 15.5m, 3", 45deg).
AS Cas Fundamental mode period P0 is given in the Table; the
AS Cas corresponding amplitude is 0.59m. First-overtone period
AS Cas P1 = 2.2909d; amplitude of oscillations with this period
AS Cas 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 +
BD Cas 3.65129d*E (JD2415000 - 29130) [0915];
BD Cas since JD2429130 - see Table.
BE Cas VB A (B G, 25", 260deg).
BH Cas According to [0453] there are no variable stars on the
BH Cas place of BH Cas and in its surroundings.
BM Cas Min II 8.98. Shape of the light curve varies. P var.
BM Cas There is a periodic term in the elements:
BM Cas +2.6d*sin(7.11deg*E + 104deg).According to [0939], on the
BM Cas light curve cepheid-like variations are observed with
BM Cas 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.
BY Cas Max = 2416871.91 + 3.2218d*E (JD2416800 - 24860) [0921];
BY Cas Max = 2431929.60 + 3.221297d*E (JD2426900 - 34300);
BY Cas Max = 2438399.629 + 3.222588d*E (JD2436200 - 39400);
BY Cas since JD2439400 - see Table.
BZ Cas Min II 11.5.
CC Cas Min II 7.26. The light curve shape var? P var?
CE CasA Possible member of the cluster NGC 7790. VB A (B = CEb Cas,
CE CasA 2.4", 265deg).
CE CasB VB B (A = CEa Cas). Possible member of the cluster NGC 7790.
CF Cas Possible member 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
CQ Cas 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
CV Cas given in the Table. P var?
CW Cas Min II 11.47. Shape of the light curve and depths of
CW Cas minima vary. P var. Min I = 2435745.6163 + 0.31886497d*E
CW Cas (JD2432400 - 41000) [3332]; since JD2441000 - see Table.
CY Cas [A/H] = -0.7.
DD Cas P var. Max = 2415612.45 + 9.807272d*E (JD2415600 - 18600);
DD Cas since JD2418600 - see Table. The star may be a member of a
DD Cas 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);
DI Cas 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
EM Cas 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
EQ Cas (JD2432200 - 34060) [3336]; since JD2436100 - see Table.
EY Cas Min II 14.5.
GG Cas d = 0.013P. Min II 9.99. P var? Min I = 2430188.468 +
GG Cas 3.758738d*E (JD2424800 - 39500) [0936];
GG Cas 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
GU Cas (JD2417470 - 35480) [0941];
GU Cas Min I = 2437367.375 + 3.09325d*E (JD2435480 - 38750) [0001];
GU Cas since JD2438750 - see Table.
GZ Cas Mean magnitude varies with P = 800d.
GZ Cas 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;
HT Cas D = 0.13P. Depth of eclipses between outbursts is ~2.4 V.
HT Cas Small quasi-periodic light oscillations with P = 100s.
HT Cas Spectrum description [6163].
HU Cas P var. Max = 2417525.075 + 0.41159875d*E (JD2411600 -
HU Cas 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 +
IR Cas 0.68069178d*E (JD2417500 - 38400) [0098];
IR Cas since JD2438400 - see Table.
IS Cas Min II 12.2. P var. Min I = 2428776.262 +
IS Cas 1.8415172d*E (JD2417400 - 29500) [0098];
IS Cas since JD2428000 - see Table.
IT Cas Min II 11.8; Min II - Min I = 0.553P; DII = 0.042P.
IT Cas Apsidal motion is possible.
IV Cas Min II 11.3. P var. Min I = 2428991.302 +
IV Cas 0.9985232d*E (JD2416700 - 29000) [0098];
IV Cas Min I = 2431438.648 + 0.9985056d*E (JD2429000 -
IV Cas 37700) [2263]; since JD2440000 - see Table.
IW Cas S4 +/6e.
IX Cas P var. Max = 2428749.39 + 9.15035d*E (JD2414700 -
IX Cas 29500) [0098]; Max = 2428749.90 + 9.1363d*E
IX Cas (JD2428700 - 34350) [0944]; Max = 2437195.642 +
IX Cas 9.14783d*E (JD2434350 - 39100) [5462];
IX Cas since JD2442000 - see Table. [A/H] = -0.4.
KL Cas Min II 12.3.
KO Cas P var. Max = 2425590 + 305.6d*E (JD2416700 - 26000);
KO Cas since JD2426000 - see Table.
KR Cas Min II 9.9.
LR Cas Min II 10.9.
LU Cas Min II 14.3?
LW Cas In the apex of a small (8") bright cometary nebula in the
LW Cas region of IC 1848. Novalike outburst was observed in the
LW Cas interval JD2433900 - 34800. Infrared and radioemission.
LX Cas In the region of the cluster Collinder 33. Min II 15.3;
LX Cas Min II - Min I = 0.47P; dI = 0.10P.
LY Cas In the region of the cluster Collinder 33. Min II 15.2.
MM Cas d = 0.08P: Min II 12.4.
MN Cas Min II 10.57.
MO Cas In the nebula NGC 7635. 10.2 - 13.1 I.
MP Cas In the nebula NGC 7635. 10.4 - 13.5 I.
MR Cas Min II 15.5.
MS Cas Min II 13.2.
MT Cas d = 0.04P. Min II 14.02.
MU Cas Min II 10.8.
MV Cas Min II 14.0.
MY Cas Min II 15.2. P var. Elements given in the Table are valid
MY Cas since JD2438500.
NN Cas Min II 14.0.
NT Cas Min II 14.4.
NU Cas Min II 13.4.
NV Cas d = 0.03P.
OP Cas P var. Max = 2429109.726 + 5.510019d*E (JD2427950 - 34670)
OP Cas [0176]; since JD2437000 - see Table.
OR Cas Min II 11.8. P var. Min I = 2429249.424 + 1.2457026d*E
OR Cas (JD2413800 - 34800) [0176]; since JD2432000 - see Table.
OX Cas In the region of the cluster NGC 381. d = 0.016P. Min II
OX Cas 10.30; Min II - Min I = 0.512P. Apsidal motion [4524].
PR Cas P = 171d?
PV Cas Min II 10.36; Min II - Min I = 0.480P.
PV Cas Depth of Minima probably varies. P var. Min I =
PV Cas 2428796.8142 + 1.75047346d*E (JD2415700 - 40000) [5302];
PV Cas since JD2440000 - see Table. Apsidal motion [6253]:
PV Cas Min II = 2428797.6894 + 1.75047346d*E -
PV Cas 0.040d*sin(0.0075deg*(E - 3000)).
PX Cas Min II 15.0.
PY Cas Epoch of Min brighness is given. Similar to RV Tau by
PY Cas light curve shape [3348].
PZ Cas VB A (B 12.8m, WN 8:, 15", 100deg). OH, H2O emission.
QQ Cas Min II 10.8. P var. Min I = 2434330.169 + 2.142030d*E
QQ Cas (JD2415700 - 30000) [2530]; since JD2430000 - see Table.
QX Cas In the region of the cluster NGC 7790. VB A (B 13.1m, 3").
QX Cas Min II 10.50; Min II - Min I = 0.37P; DII = 0.047P;
QX Cas dII = 0.018P.
V0336 Cas Min II 13.6.
V0341 Cas d = 0.031P.
V0344 Cas Min II 13.4.
V0345 Cas Min II 13.6.
V0346 Cas The coordinates refer to the sp component of a wide pair,
V0346 Cas whereas the chart [2345] leads to the nf component. It is
V0346 Cas the sp component that is red and probably var.
V0357 Cas Min II 13.6.
V0359 Cas Min II 12.0.
V0360 Cas Min II 12.3.
V0361 Cas d = 0.051P.
V0363 Cas Delta(S) = 1.
V0364 Cas Min II 11.9.
V0365 Cas S6/3- .
V0366 Cas Min II 12.7. P var. Min I = 2435075.461 + 0.7292714d*E
V0366 Cas (JD2414600 - 35400) [2305]; since JD2434650 - see Table.
V0373 Cas An unique close binary. Porb = 13.4192d [4627]. Epoch
V0373 Cas of Min I is given close to the epoch of one of
V0373 Cas conjunctions. Min II - Min I = 0.58P. Maxima are very
V0373 Cas sharp. Max - Min II = 0.25P. It is not excluded that the
V0373 Cas star is an eclipsing one with physical variability of
V0373 Cas components, but eclipses, if they exist, cause only a very
V0373 Cas small part of the observed light variations. Range of
V0373 Cas light variations is given according to [2651]. As a rule
V0373 Cas the amplitude is close to 0.1m.
V0374 Cas Min II 12.1.
V0375 Cas Min II 10.6.
V0377 Cas VB (A 8.5m; B 9.4m, 2.1", 185deg, 1962).It is not known
V0377 Cas which component varies. According to [4005] the range
V0377 Cas of combined brightness variations is 0.26m.
V0377 Cas According to [7051], const.
V0380 Cas d = 0.08P.
V0381 Cas Min II 10.8.
V0388 Cas Wolf 47 (mu = 0.82", p = 80deg). Faint component of a wide
V0388 Cas physical pair (p = 294") the bright component of
V0388 Cas which is the dM2 star Wolf 46 = BD+61deg 195 (9.4).
V0392 Cas Min II 14.0. P var. Min I = 2429640.390 +
V0392 Cas 4.54094d*E (JD2425300 - 29640); Min I =
V0392 Cas 2429640.390 + 4.54064d*E (JD2429640 - 36900) [4027];
V0392 Cas since JD2436900 - see Table. Depth of Min var?
V0394 Cas Min II 15.6.
V0396 Cas Min II 10.2.
V0399 Cas Min II 14.1.
V0401 Cas Min II 15.7.
V0402 Cas Min II 15.3.
V0406 Cas Min II 16.8.
V0410 Cas Bright in 1938 -39. Slow. Not red.
V0423 Cas Min II 14.3.
V0427 Cas Min II 13.7.
V0428 Cas Red.
V0430 Cas Northern component of a close pair. Red.
V0434 Cas Red.
V0441 Cas P = 351.2d?
V0442 Cas d = 0.025P. P var? Since 1972 P = 3.592120d.
V0444 Cas Min II 16.0. P var. Min I = 2438651.314 + 2.224808d*E
V0444 Cas (JD2432850 - 37300); since JD2437300 - see Table. Period
V0444 Cas variation may be cyclic. Mean elements:
V0444 Cas Min I = 2443194.258 + 2.224773d*E.
V0445 Cas Min II 11.08.
V0448 Cas Min II 15.0.
V0450 Cas VB A (B 17.5m:, 3.4", 188deg). Range
V0450 Cas of combined light variations is given.
V0459 Cas Min II 11.6.
V0466 Cas In the region of the cluster NGC 457.
V0480 Cas Min II 14.7.
V0482 Cas VB A (B 10.0m, F 4 V, 6", 195deg; optical). P = 0.28292d?
V0497 Cas In the region of the cluster IC 1848.
V0498 Cas In the region of the cluster IC 1848.
V0499 Cas In the region of the cluster IC 1848.
V0509 Cas Pulsation of photosphere with P = 3 years.
V0509 Cas Tenuous shell ejected in 1975 is now falling back to
V0509 Cas the star.
V0518 Cas In the region of the cluster Stock 2. Star N136 (Stock 208).
V0520 Cas Min II 13.1. P var. Min I = 2439069.559 + 0.489832d*E
V0520 Cas (JD2438580 - 40850); since JD2441150 - see Table.
V0521 Cas Member of the cluster NGC 7789.
V0523 Cas Min II 11.34. P var. Min I = 2432054.555 +
V0523 Cas 0.2336882d*E (JD2428545 - 33570) [7008];
V0523 Cas Min I = 2439029.461 + 0.23368912d*E (JD2439000 - 41300)
V0523 Cas [7387]; since JD2440480 - see Table.
V0524 Cas OH, H2O emission. P = 163d?, 191d? 259d?, 620d?
V0526 Cas Two oscillations are superimposed: P1 = 0.0526d (A1 =
V0526 Cas 0.0036m), P2 = 0.0396d (A2 = 0.0056m); P2/P1 = 0.753.
V0527 Cas Min II 13.5; Min II - Min I = 0.52P.
V0532 Cas In the region of the cluster NGC 7789.
V0533 Cas In the region of the cluster NGC 7789.
V0536 Cas P var. Max = 2438700.262 + 0.395674d*E
V0536 Cas (JD2438580 - 39150); Max = 2441186.333 +
V0536 Cas 0.395683D*E (JD2440070 - 41250);
V0536 Cas since JD2441500 - see Table.
V0540 Cas Epoch of Max (U) is given.
V0541 Cas Min II 11.0.
V0542 Cas In the region of the cluster NGC 7789.
V0544 Cas Elements given in the Table are valid since JD2428000.
V0546 Cas In the region of the cluster NGC 103. Min II 14.8.
V0547 Cas VB A (B 12.4m, M4.5, 2.8", 93deg). Astrometric binary
V0547 Cas (A = 0.12", P = 15.9a); mu = 1.75", P = 98deg.
V0547 Cas Variation of combined light is given.
V0551 Cas P = 45.5d?/57d?/67.5d?.
V0554 Cas P >= 3500d? D = 400d?
V0559 Cas VB A (B 7.7m, 0.25", 34deg, 1976). Min II 7.21.
V0566 Cas VB A (B 8.3m, 1.4", 194deg, 1965).
V0569 Cas 10.0 - 14.7 I.
V0589 Cas In the cluster NGC 663.
V0592 Cas White dwarf. Rapid non-periodic fluctuations of brightness
V0592 Cas on a time scale of several minutes.
V0598 Cas VB A (B 12m, 19", 0deg). P = 2.825d? [2560].
V0615 Cas Variable radio source on 10.5 GHz; gamma - and X-ray
V0615 Cas source?
V0627 Cas H2O emission.
V0635 Cas 4U 0115 + 634. SB (P = 24.3162d).
V0635 Cas Pulsar period P = 3.6136s.
V0638 Cas Epoch of Min is given.
V0742 Cas SB, Porb = 55.9212d.
V0745 Cas Component B of the double system observed brighter than in the
V0745 Cas Hipparcos Input Catalogue.
V0746 Cas SB, Porb = 27.8d.
V0747 Cas VB. The variability may be due to the fainter component.
alf Cas VB A (B 14.5m, 17.6", 272deg; C 13.5m, 38", 105deg;
alf Cas D 8.5m, 64.4", 280deg.)
bet Cas VB A (B 13.7m, 31.3", 243deg); SB (P = 27d).
bet Cas [Fe/H] = 0.64.
gam Cas VB A (B 11.0m, 2.2", 248deg; C 13.0m, 52.2", 348deg).
gam Cas In HII region S 185. X-ray source MX 0053 + 60.
gam Cas v sin i = 310 km/s.
del Cas VB A (B 11.5m, 31.7", 66deg). Min II 2.75. Min II - Min I =
del Cas 361d. The elements given in the Table are still not
del Cas confirmed by anyone.
iot Cas VB A (B 6.89m, 2.3", 239deg; C 8.40m, 7.2", 114deg).
iot Cas Astrometric binary (a = 0.113", P = 52.4a). Max (V) - Max
iot Cas (lambda 1550) = 0.4P; A (lambda 1550) = 0.40m. The range
iot Cas of total brightness variation of components A and
iot Cas B is given.
kap Cas P = 0.09028d, P(Vr) = 0.14035d [2588]; P = 7d [8876].
omi Cas VB A (B 11.7m, 33.6", 303deg). SB1 (P = 1033d);
omi Cas V sin I = 220 km/s.
pi Cas SB, Porb = 1.9642d.
rho Cas Usually varies within the limits 4.4m - 5.2m V.
rho Cas In November 1945 the peculiar decrease of brightness began
rho Cas lasting for 165d and in September 1946 the star reached
rho Cas the middle of the deepest minimum (JD2432070) lasting for
rho Cas 320d. Then the brightness began to increase symmetrically
rho Cas and by July 1947 the star attained its normal brightness
rho Cas [0957]. Photographic magnitudes varied in the limits
rho Cas 5.4m - 8.3m. Spectrum description [8878].
B Cas Tycho Brahe's supernova. Stellar object is not identified
B Cas optically up to now.
R Cen VB A (B 12m, 28", 218deg). Epoch
R Cen of Min I is given. Min I 0.00P, Max I 0.23P, Min II
R Cen 0.47P, Max II 0.64P. 5.8, 6.0,
R Cen 11.1, 8.3. P var. P = 561.3d
R Cen before 1918; since 1918 - see Table. H2O maser.
V Cen In the field of the open cluster NGC 5662.
Z Cen SN 1895 (NGC 5253).
RR Cen Min II 7.63. dII = 0.08P. P var. Min I = 2424231.0910 +
RR Cen 0.60568807d*E + 2.31d*10**(-10)*E**2 (JD2414170 -
RR Cen 33470) [0006]. Current elements - see Table.
RS Cen A 1118-61?
RT Cen P var.
RZ Cen Min II 9.4.
SS Cen Min II 9.5.
ST Cen Min II 11.30, DII = 0.22P. Max II (before
ST Cen Min I) 10.65.
SU Cen Min II 9.2.
SV Cen Min II 9.45. Delta(m) var. P var. Min = 2433053.358 +
SV Cen 1.6594795d*E - 7.61d*10**(-8)*E**2 (JD2412608 - 42097).
SV Cen Cyclic (32a - 33.6a) period variations were noted in
SV Cen [0009, 5212]. Since 1978 - see Table. P Cyg profiles in
SV Cen the spectrum.
SX Cen For mean light Max = 2426835 + 615d*E.
SY Cen d = 0.05P.
SZ Cen VB. Min II 8.7.
TX Cen VB? B - V: +1.39, +2.11.
TZ Cen The co-ordinates in the Table are based on [0015].
TZ Cen According to [0016], no star brighter than 14m was found
TZ Cen in this position. The co-ordinates in [0015] may be in
TZ Cen error.
UW Cen IR excess.In Max varies semiregularly, P ~42d [8832].
UZ Cen VB A (B 13.8m, 4", 191deg). Max II = 2440746.2 +
UZ Cen 2.35529d*E.
VW Cen VB A (B ~15m?, ~8", ~180deg). B - V: +1.01, +1.71.
VW Cen [A/H] = 0.3.
VZ Cen Min II 8.4.
WX Cen ~ +0.45, ~ -0.72.
WX Cen Proposed as an optical counterpart of the transient X-ray
WX Cen source Cen X-2 [5314], though no optical bursts were
WX Cen observed.
WZ Cen Min II 14.2.
ZZ Cen VB C (A 9.4m, B9; B 10.8m, 8", 314deg; C = ZZ Cen,
ZZ Cen 9", 259deg; D = AA Cen, 9", 110deg).
AA Cen VB D (see ZZ Cen).
AB Cen d = 0.05P.
AP Cen Epoch of Min is given.
AS Cen Min II 13.2.
AV Cen Min II 14.1.
AZ Cen The shape of the light curve varies.
BD Cen Min II 10.7.
BF Cen In the field of the open cluster NGC 3766. Min II 8.8.
BG Cen Min II 12.3.
BH Cen In the open cluster IC 2994. Min II 8.8.
BI Cen Delta(S) = 2.
BK Cen P2 = 2.236d, A1 = 0.54m, A2 = 0.22m [8835].
BV Cen The mean cycle between outbursts <= 149.4d [7301]. The
BV Cen tabulated elements correspond to Max of the eclipsing
BV Cen light curve, phi (Min) = 0.25P. The range of the eclipsing
BV Cen variability is 12.8 - 13.3.
CN Cen Min II 13.3.
DI Cen Min II 12.3, Min II - Min I = 0.494P, DII = 0.08P:.
DT Cen Red.
DX Cen The P star in a pair.
DY Cen All spectral lines are very weak. No IR excess. The
DY Cen photometric behaviour outside major Min is described in
DY Cen [8836].
EP Cen Min II 11.5.
EU Cen The P star in a pair.
GI Cen In the field of the globular cluster NGC 5286.
GM Cen The chart in [6286] is wrong.
IQ Cen d = 0.04P.
IW Cen Min II 12.1.
IX Cen In the field of the open cluster NGC 3706.
IY Cen In the field of the open cluster IC 2944.
IZ Cen = 1.7.
KK Cen B - V: +1.08, +1.62.
KM Cen Min II 13.3.
KN Cen B - V: +1.36, +1.75. [A/H] = 0.2.
KQ Cen Alternating periods 136d, 159d.
KT Cen B - V: +0.46. Min II 12.72. Min II - Min I = 0.392P
KT Cen (JD2441686 - 721); apsidal motion is observed [8094].
KY Cen Min II 13.3.
KZ Cen B - V: +0.30, +0.72.
LL Cen Min II 13.1.
LR Cen Min II 12.30.
LT Cen Min II 9.6.
LU Cen The period may be twice longer.
LV Cen B - V: +1.3, +1.7.
LW Cen Min II 9.6. In the field of the open cluster IC 2944.
LX Cen Min II 13.55.
LZ Cen Min II 8.50.
MM Cen Min II 12.7.
MN Cen Min II 8.7. VB A (B 10.9m, 7", 147deg).
MP Cen Min II 10.0.
MQ Cen Min II 10.1.
MR Cen Min II 10.5.
MV Cen Min II 14.6.
MY Cen B - V: +1.58, +1.94.
NO Cen Min II 14.2.
NP Cen Min II 10.2.
NY Cen Min II 11.9.
OO Cen = 1.84.
OP Cen Min II 13.8.
OU Cen Min II 10.9.
OV Cen Min II 11.0.
OX Cen Min II 14.3.
QS Cen d = 0.03P.
QT Cen Min II 13.4.
QY Cen = 2.16.
QZ Cen P var? The shape of the light curve varies?
V0339 Cen VB A (B ~13m, SP). B - V: +1.08, +1.47.
V0343 Cen Min II 13.5.
V0344 Cen Min II 12.3.
V0346 Cen In the field of the open cluster Stock 14. Min II 8.8.
V0346 Cen Min II = 2421966.835 + 6.32189d*E.
V0348 Cen d = 0.010P.
V0349 Cen Min II 14.5.
V0350 Cen Min II 10.3. Min II = 2430870.192 + 3.216906d*E.
V0351 Cen Epoch of Min is given.
V0356 Cen Min II 15.0.
V0358 Cen Epoch of Min is given.
V0365 Cen d = 0.040P.
V0373 Cen VB A (B ~4" np).
V0377 Cen d = 0.003P.
V0379 Cen Min II 8.9.
V0380 Cen Min II 10.0.
V0383 Cen Min II 13.6:, Min II - Min I = 0.609P.
V0384 Cen Min II 12.2. DII = 0.062P. Min II - Min I = 0.667P.
V0385 Cen Min II 13.0.
V0388 Cen Min II 15.7.
V0399 Cen d = 0.020P. Min II 13.1.
V0405 Cen P var, 30d - 40d.
V0412 Cen VB A (B 59", 266deg).
V0419 Cen P var. Max = 2428099.25 + 5.50713d*E (JD2428099 - 33573);
V0419 Cen since JD2434900 - see Table.
V0420 Cen B - V: +0.45, +0.97. P var. Nonlinear term:
V0420 Cen -0.000090d*E**2.
V0427 Cen Epoch of Min is given.
V0436 Cen SB (P = 0.0669d). Photometric P during supermaxima
V0436 Cen 0.06383d [8838]. Rapid oscillations in supermaxima
V0436 Cen Delta(m) ~0.002m, P ~19.6s [8049].
V0440 Cen d = 0.033P. Min II is possible.
V0443 Cen d = 0.025P.
V0491 Cen Very flat minima; close companion?
V0495 Cen d = 0.042P. Min II 10.6. Min II - Min I = 0.520P.
V0496 Cen Possible member of the open cluster NGC 4755.
V0496 Cen B - V: +1.02, +1.33.
V0498 Cen P may be twice shorter.
V0499 Cen (k - b)2 = 0.23.
V0504 Cen Semiregular variations (P1 ~130d, P2 ~411d)
V0504 Cen are also observed [8836].
V0506 Cen The chart in [6286] is wrong.
V0508 Cen Min II 13.2.
V0526 Cen Delta(m) var. P var. Max = 2425707.540 + 0.56153d*E
V0526 Cen (1929 - 1930); during 1931 - 1940 - see Table.
V0527 Cen The chart in [6286] is wrong.
V0532 Cen Star 1 [9078]. X-ray source 3A 1431-409.
V0544 Cen 2AS E 1440-39? [5962]. The chart in [6286] is wrong.
V0545 Cen Magnitude in Max var (12.6 - 14.5), P = 1800d?
V0553 Cen [Fe/H] = -0.1; [C/Fe] = +0.8.
V0565 Cen Min II 13.9. Type RR is not excluded (P = 0.238072d).
V0574 Cen sp star of a pair.
V0577 Cen According to improved coordinates, the star is actually in
V0577 Cen Hydra.
V0585 Cen Min II 13.0.
V0592 Cen Mean brightness var.
V0593 Cen Possible member of the open cluster Stock 16. Min II 11.2.
V0594 Cen V133 (omega Cen); non-member of the cluster. Min II 14.4.
V0606 Cen Min II 9.8.
V0607 Cen Min II 14.1.
V0608 Cen Min II 13.1.
V0609 Cen Min II 13.6.
V0615 Cen Min II 14.0.
V0617 Cen Min II 13.8:.
V0619 Cen In the field of the open cluster NGC 5316.
V0621 Cen d = 0.05P.
V0624 Cen Min II 14.9.
V0625 Cen Min II 15.0.
V0627 Cen d = 0.02P.
V0628 Cen Min II 13.2.
V0630 Cen Min II 14.2. d = 0.06P.
V0635 Cen Min II 13.9.
V0636 Cen Min II 8.8.
V0644 Cen During the faint phase in 1951 the shell spectrum was
V0644 Cen observed [2128]. Type E with a very long period is
V0644 Cen possible [6763].
V0645 Cen Proxima Cen = alpha Cen C. mu = 3.809", P = 281.7deg.
V0645 Cen Soft X-ray source.
V0646 Cen d = 0.022P. Min II 9.1.
V0662 Cen P ~2.48d or 2.95d.
V0672 Cen Min II 11.4 - 11.6 (var).
V0673 Cen Depth of Min II 0.05m.
V0674 Cen Blazhko effect: Pi = 29.5d. 0.15P <= M - m <= 0.23P.
V0676 Cen Min II 12.5.
V0677 Cen Min II 11.6.
V0678 Cen Min II 10.6.
V0679 Cen 9.8"p, 1.1"n from CPD -62deg 2167.
V0679 Cen The star is at the edge of a dark cloud in a bright nebula,
V0679 Cen a part of IC 2944, in the field of a very poor open
V0679 Cen cluster. Since 1950 till 1954 faded by 2.5m. Rather red.
V0679 Cen "Screening" by the edge of a dark nebula?
V0682 Cen IR excess.
V0684 Cen Depth of Min II 0.05m.
V0685 Cen Min II 9.5.
V0686 Cen RV type is not excluded.
V0687 Cen Min II 14.1. DII = 0.12P. Min II - Min I = 0.580P.
V0688 Cen Min II 12.7.
V0689 Cen Min II 12.1.
V0690 Cen Depth of Min II 0.03m.
V0692 Cen Min II 11.6. Min II - Min I = 0.481P.
V0701 Cen VB? d = 0.026P. Min II 9.1.
V0704 Cen IR excess.
V0716 Cen Min II 6.21.
V0742 Cen Min II 10.1.
V0743 Cen (k - b)2 = 0.20. Elements almost as well satisfactory:
V0743 Cen Max = 2439243.6465 + 0.10222560d*E.
V0745 Cen Min II 9.6.
V0746 Cen = V467 Cen. Marked as V467 Cen in the chart.
V0747 Cen Min II 10.05.
V0748 Cen B - V: +0.31, +1.21; U - B: -0.66, -0.21. d = 0.106P.
V0748 Cen Narrow Halpha emission. Outside eclipses shows variations
V0748 Cen by 0.05m - 0.1m during several days or several weeks
V0748 Cen (probably irregularly) [6968].
V0752 Cen Min II 9.61. dI = dII = 0.047P.
V0753 Cen (k - b)2 = 0.20. In the field of the open cluster NGC 3960;
V0753 Cen probably non-member. Type DSCT is possible.
V0754 Cen Slight Min II.
V0755 Cen In the Coalsack.
V0756 Cen In the Coalsack. High excitation lines (OVII, OVIII, CV)
V0756 Cen are present in the spectrum. WR type is possible [7372].
V0757 Cen Min II 8.6.
V0758 Cen d = 0.07P. Min II 9.15.
V0759 Cen Min II 7.56.
V0761 Cen IR excess.
V0763 Cen VB A (B 13m, 7", 163deg).
V0766 Cen VB A (B 10.01m, B0Ibp, 9", 318deg). IR excess.
V0767 Cen VB A (B 11.52m, 21", 350deg).
V0768 Cen Possible P: 60d - 80d.
V0770 Cen According to [7570], const?
V0772 Cen In the region of the open cluster IC 2944.
V0775 Cen EB type is possible. Deep Min II.
V0777 Cen Deep Min II.
V0779 Cen Cen X-3 (3U 1118-60). : +1.04; : -0.08.
V0779 Cen Min II 13.39. Porb var. The shape of the light curve
V0779 Cen varies. Epoch of Min I is given. Epochs of Min II coincide
V0779 Cen with the moments of X-ray eclipses. X-ray pulses are
V0779 Cen observed with Ppuls = 4.834477s (epoch JD2442785.3);
V0779 Cen Ppuls decreases [7612]. No rapid optical oscillations
V0779 Cen were found.
V0783 Cen B - V: +0.35.
V0784 Cen Very red.
V0788 Cen Min II 5.90.
V0790 Cen VB B (A 4.52m; 60", 343deg).
V0791 Cen In the region of globular cluster omega Cen (NGC 5139).
V0791 Cen Cluster non-member.
V0795 Cen VB A (B 12.29m, 33.9", 170deg; C 12.79m, 36", 220deg).
V0801 Cen 4U 1145 - 61 = 2S 1145 - 619. Primary component has a low
V0801 Cen density envelope expanding with the velocity of 1800 km/s.
V0801 Cen V sin i = 290 km/s. X-ray pulsar (P = 291.8s
V0801 Cen [8883]). Max (X) = 2442519.5 + 187.5d*E [8881].
V0803 Cen Extremely hot hydrogen-deficient helium star.
V0807 Cen VB (9.9m, 10.1m, 0.4", 258deg, 1931).
V0807 Cen It is not known which of the components varies.
V0810 Cen Member of the cluster Stock 14.
V0813 Cen In the region of globular cluster omega Cen (NGC 5139).
V0813 Cen V65 (NGC 5139).
V0814 Cen In the region of globular cluster omega Cen (NGC 5139).
V0814 Cen V78 (NGC 5139). Min II 14.165:. Primary
V0814 Cen component is probably intrinsically variable [8884].
V0816 Cen Primary oscillation is superimposed by the oscillations
V0816 Cen with freguencies: F2 = 4.9229, F3 = 4.7343, F4 = 4.9317
V0816 Cen [2591].
V0820 Cen [Fe/H] = -2.5; Vr = +260 km/s.
V0822 Cen Cen X-4.
V0825 Cen In the region of globular cluster omega Cen (NGC 5139).
V0825 Cen Cluster non-member. V2 (NGC 5139).
V0826 Cen In the region of globular cluster omega Cen (NGC 5139).
V0826 Cen Cluster non-member. V129 (NGC 5139).
V0902 Cen VB, rho = 12". Variability may be spurious.
V0915 Cen The variability type is not quite consistent with the spectral
V0915 Cen type (B9II/III).
V0921 Cen High proper motion (LTT 4397) not confirmed by HIPPARCOS data.
V0933 Cen HIPPARCOS data contradict the luminosity class V.
V1015 Cen Variability type and luminosity class (III) do not agree.
bet Cen VB A (B 4.1m, 1.3", 251deg, 1960). SB1 (P = 352d
bet Cen [8887]. Multiperiodicity; sometimes brightness is constant
bet Cen [8215]. Soft X-ray source.
del Cen VB A (B 4.8m, 68.6", 325deg; C 6.5m, 16.6", 227deg).
eps Cen VB A (B 13.0m, 36.0", 158deg). There is a secondary light
eps Cen oscillation with the amplitude of 0.0034m and elements:
eps Cen Max = 2441041.058 + 0.17696d*E.
eta Cen VB A (B 13.5m, 5.6", 270deg, 1897); SB?
mu Cen VB A (B 13.63m, 48", 128deg).
omi 1 Cen VB A (B 11.4m, 13.5", 125deg).
T Cep P var. Max = 2414252 + 386.05d*E (JD2406900 - 20490);
T Cep Max = 2431086 + 394.93d*E (JD2420490 - 32900);
T Cep Max = 2440262 + 379.22d*E (JD2432900 - 42200); since
T Cep JD2442200 Max = 2444171 + 392.7d*E. Mean value of the
T Cep period is given in the Table. SiO maser.
U Cep VB A (B 11.83m, 13.9", 62deg; C 12.3m, 23.0", 318deg).
U Cep 0.010P <= d <= 0.040P. Min II 6.93. P var. Min I =
U Cep 2407890.3346 + 2.4928551d*E + 5.15d*10**(-9)*E**2
U Cep (JD2388855 - 2440790) [6468]; analysis of period
U Cep variations in this interval see also in [7395];
U Cep Min I = 2441395.3604 + 2.4931048d*E (JD2440790 - 41600);
U Cep Min I = 2441679.5716 + 2.4930432d*E (JD2441600 - 950);
U Cep Min I = 2443753.7982 + 2.4930679d*E (JD2442100 - 43800);
U Cep since JD2444000 - see Table. Shape of the light curve
U Cep and depth of minima vary. Brightness of the secondary (G8)
U Cep varies sporadically. Subgiant brightening accompanies
U Cep eruptive mass transfer. The gaseous stream moving to the
U Cep primary (B7) component forms around it gaseous ring or
U Cep disc [8889].
W Cep Slow oscillations with Pi ~2000d are superimposed by
W Cep oscillations with P ~350d.
X Cep OH emission?
RS Cep d = 0.039P. P var. Min = 2417140.469 + 12.419925d*E
RS Cep (JD2410000 - 31000) [2431]; since JD2431000 - see Table.
RZ Cep P var. Max = 2411640.654 + 0.308697d*E
RZ Cep (JD2411640 - 15000); Max = 2417144.620 + 0.3086203d*E
RZ Cep (JD2415600 - 20200); Max = 2421175.611 +
RZ Cep 0.3086699d*E (JD2421175 - 23000); Max =
RZ Cep 2423768.475 + 0.3086918d*E (JD2423000 - 31700);
RZ Cep Max = 2433768.493 + 0.3086383d*E (JD2433700 -
RZ Cep 38300) [8890]; Max = 2438207.938 + 0.308645d*E
RZ Cep (JD2438200 - 39040) [3879]; Max = 2440834.579 +
RZ Cep 0.3086735d*E (JD2440800 - 42640) [8890];
RZ Cep since JD2442640 - see Table. Shape of the light curve and
RZ Cep the amplitude A vary with the Blazhko effect period
RZ Cep Pb = 96.8*P0 = 29.88d; Min A = 2441464.147 + 29.88d*N
RZ Cep [8891]. Long period variation of P0 with a period ~50
RZ Cep years is possible. Delta(S) = 6.
SS Cep Mean brightness varies with cycles from some hundreds to
SS Cep thousands days.
SU Cep Min II 10.6.
SV Cep IR excess.
SX Cep In the region of the nebula NGC 7023.
SY Cep Min II 12.70. P var?
SZ Cep VB A (B 12.3m, 24.9", 263deg). S4/6e.
TT Cep VB A (B 17.0m, 8", 160deg).
TY Cep Epoch of Min I is given.
UZ Cep P var. Max = 2440969 + 297.68d*E (JD2414000 - 42000);
UZ Cep since JD2440000 - see Table.
VV Cep VB (0.05", 174deg, 1950)? 0.066P <= D <= 0.091P;
VV Cep 0.040P <= d <= 0.077P. Depth of eclipses: 2.30m (lambda
VV Cep 3500 A), 1.9m (U), 0.4m (B). M-component is of SRC type:
VV Cep Max = 2443045 + 118.37d*E [8698, 8894]; A(V) <= 0.33m.
VV Cep Light oscillations are also noted with P ~58d [8895],
VV Cep 25d and 150d [8896]. B-component may be also an intrinsic
VV Cep variable [2416]. Gaseous streams. Strong variable magnetic
VV Cep field.
VW Cep VB A (B 10.3m, a = 0.51", P = 30.45a [8897]); mu alpha =
VW Cep +0.0899s, mu delta = +0.560". Min II 7.56.
VW Cep Shape of the light curve and depths of Min I and Min II
VW Cep vary. P var. Min I = 2433483.4257 + 0.27831758d*E +
VW Cep 0.050d*cos(0.004813deg*(E - 4700)) (JD2424763 - 41200)
VW Cep [6483]; since JD2441000 - see Table. Period
VW Cep change study see also in [8899]. X-ray source.
VZ Cep Min II 9.93.
WX Cep Min II 9.14; dI = 0.01P, dII = 0.00P.
WY Cep Min II 11.5. P var [2545].
WZ Cep Min II 11.9.
XX Cep Min II 9.26. P var. Min I = 2425096.449 + 2.337340d*E
XX Cep (JD2414930 - 30000); Min I = 2441539.4917 + 2.3373059d*E
XX Cep (JD2430000 - 42300) [8902]. Since JD2441500 - see Table.
XY Cep Min II 10.10. P var?
XZ Cep Min II 8.43.
ZZ Cep VB A (B 10.2m, A2 P, 3.6", 202deg; C 10.87m, A5V,
ZZ Cep 20.6", 219deg). Min II 8.74.
AH Cep Min II 7.03. Depth of minima varies. P var.
AH Cep Min I = 2434989.3702 + 1.7747274d*E (JD2415500 - 35000)
AH Cep [3604]; since JD2434900 - see Table: +3.12d*10**(-9)*E**2.
AI Cep Min II 9.48.
AN Cep Since JD2425200 primary and secondary maxima and minima
AN Cep appeared, and mean cycle became 254d.
AV Cep d <= 0.04P.
BB Cep d = 0.050P.
BE Cep Min II 13.0.
BF Cep P var. Max = 2437236 + 426.11d*E (JD2423600 - 37300);
BF Cep Max = 2441665 + 442.3d*E (JD2437300 - 42500); since
BF Cep JD2442500 - see Table.
BH Cep Sometimes strong Algol-like light weakenings are observed.
BO Cep Sometimes strong Algol-like light weakenings are observed.
CO Cep Min II 12.6; Min II - Min I = 0.552P; DII = 0.080P.
CP Cep P var?
CQ Cep Shape of the light curve and depth of minima vary.
CQ Cep According to [7401] on 1969 March 28/29 on the phase
CQ Cep 0.56P a light decrease by 0.1m was observed and then a
CQ Cep rapid flare by 0.35m U, 0.13m B, 0.14m V. P var. Nonlinear
CQ Cep term: -10**(-9)*E**2.
CR Cep P var. Max = 2436846.94 + 6.23318d*E (JD2415000 - 30000)
CR Cep [3157]; since JD2430000 - see Table.
CV Cep S7/1.5. Mean brightness varies with a cycle ~2000d [0159].
CW Cep VB A (B 12.29m, 20", 310deg). Min II 8.01;
CW Cep Min II - Min I = 0.478P (1972 yr). There is a sinusoidal
CW Cep term in the elements: +0.0250d*sin(0.0626deg*E - 28.3deg).
CW Cep Apsidal motion with P = 43a.
CX Cep Min II 12.16.
CY Cep Min II 16.5.
DD Cep P var. Max = 2427960 + 167.6d*E (JD2427900 - 30000);
DD Cep Max = 2429968 + 173.0d*E (JD2429900 - 33600);
DD Cep since JD2433600 - see Table.
DH Cep In the region of the cluster NGC 7380. Apsidal motion with
DH Cep P = 2.6a [0165].
DK Cep Min II 12.4.
DL Cep Min II 12.7.
DO Cep VB B (A 9.87m, M4V; a = 2,4", P = 44.78a, e = 0.408);
DO Cep mu = 0.852", P = 242.6deg.
DP Cep Min II 14.4.
DQ Cep Multiperiodicity: P0 = 0.12420d: [8137], P1 = 0.061177d
DQ Cep [8914].
DX Cep P var. Max = 2430603.712 + 0.5260395d*E (JD2415700 - 31000)
DX Cep [0001]; since JD2431000 - see Table. Delta(S) = 7.
DY Cep Min II 11.8.
EE Cep A var?
EF Cep Min II 12.6. P var?
EG Cep Min II 9.61. P var. Min I = 2439774.3322 + 0.54462091d*E
EG Cep (JD2415200 - 41000) [0001]; since JD2441000 - see Table.
EH Cep In the dark cloud near the diffuse nebula and the cluster
EH Cep NGC 7023.
EI Cep Min II 7.98.
EK Cep Min II 8.06; Min II - Min I = 0.545P (1965). Min II =
EK Cep 2439022.8484 + 4.427797d*E [8160].
EK Cep Apsidal motion (P = 4700a +- 600a) [8923].
EL Cep P var.
EM Cep In the region of the cluster NGC 7160. VB A (a 12.8m,
EM Cep 19.8", 281deg; B 7.9m, 62.5", 146deg). Min II 7.16.
EM Cep Shape of the light curve and depth of minima vary.
EO Cep Min II 12.3.
EP Cep In the cluster NGC 188. Min II 17.0.
EQ Cep In the cluster NGC 188. Min II 16.7.
ER Cep In the cluster NGC 188. Min II 16.27.
ES Cep In the cluster NGC 188. Min II 15.8.
ES Cep P var. Min I = 2439082.238 + 0.34468d*E (JD2438480 - 39090);
ES Cep Min I = 2439236.501 + 0.34264d*E (JD2439090 - 39280);
ES Cep Min I = 2439594.548 + 0.34250d*E (JD2439400 - 39600);
ES Cep since JD2439600 - see Table. A var.
EX Cep Min II 11.6.
EY Cep Min II 10.4.
EZ Cep P var. Max = 2416803.627 + 0.378990d*E (JD2415400 - 20000)
EZ Cep [0001]; since JD2420000 - see Table.
FH Cep Min II 12.1.
FL Cep d = 0.02P.
FS Cep Min II 12.0.
FT Cep VB A (B 18.3m, 5", 27deg). In the region of the diffuse
FT Cep nebula and the cluster NGC 7023.
FU Cep In the region of the diffuse nebula and the cluster
FU Cep NGC 7023.
FV Cep In the region of the diffuse nebula and the cluster
FV Cep NGC 7023. P = 0.4628d.
FW Cep In the region of the diffuse nebula and the cluster
FW Cep NGC 7023.
GI Cep Min II 11.9.
GK Cep Min II 7.35; dI = dII = 0.03P; Min II - Min I = 0.502P.
GK Cep P var. Min I = 2425189.526 + 0.9361614d*E
GK Cep (JD2415000 - 27500); Min I = 2438694.7070 + 0.9361714d*E
GK Cep (JD2427500 - 38200) [0001]; since JD2438200 - see Table.
GL Cep In the region of the diffuse nebula IC 1396 and the
GL Cep cluster Tr 37.
GM Cep In the region of the diffuse nebula IC 1396 and the
GM Cep cluster Tr 37.
GP Cep In the region of the HII zone S 132. Quadruple system,
GP Cep consisting of a WN6 + O8-B0III: eclipsing pair
GP Cep (P = 6.6883d) physically associated with an O + O pair
GP Cep (P = 3.4698d); the latter pair may be also an eclipsing
GP Cep or ellipsoidal variable [8931].
GS Cep Min II 10.6.
GT Cep Min II 8.6.
GW Cep Min II 12.00.
HK Cep Min II 14.4.
HZ Cep In the region of the diffuse nebula and the cluster
HZ Cep NGC 7023.
IL Cep VB A (B 11.91m, 7", 326deg); P = 2.802d?
IM Cep Min II 13.6.
IO Cep Min II 11.7.
IP Cep Min II 12.1.
IR Cep VB (Delta(m) ~0.0m, 0.0" -0.2"). P var.
IR Cep Max = 2431060.878 + 2.114016d*E (JD2428335 - 31060) [0001];
IR Cep since JD2440900 - see Table.
IV Cep VB B (A 16m; B 2.1", 191deg).
IW Cep Min II 13.7; Min II - Min I = 0.52P.
IX Cep d = 0.03P. Min II 17.0.
KL Cep d = 0.019P.
KP Cep Depth of Min II 0.03m.
KV Cep Min II 14.3.
KY Cep Flare with 65 sec duration. There is a blue object on the
KY Cep place of the flare [0001].
KZ Cep VB (8.6m, 8.6m; 1.9", 348deg). Depths of spectral lines
KZ Cep vary: P = 0.212938d [6488].
LL Cep Min II 14.0.
LM Cep Min II 12.8.
LP Cep Min II 13.8; Min II - Min I = 0.55P.
LQ Cep Eastern component of a double star.
LU Cep VB.
LW Cep Depth of Min II 0.05m.
LZ Cep Min II 5.63. In the Table: P(Vr) [4627].
MN Cep Depth of Min II 0.08m?
MQ Cep Min II 15.7.
MT Cep Min II 15.5.
MX Cep SB (P = 16.03d) [8947].
MY Cep In the cluster NGC 7419. Emission OH, H2O.
MZ Cep In the region of the cluster NGC 7419.
NN Cep Min II 8.52.
NR Cep Min II 13.6; d = 0.025P?
NS Cep Depth of Min II 0.04m.
NW Cep Preceding component of a close VB. Min II 10.7.
NY Cep VB A (B 10.33m, 10", 190deg); d = 0.003P; SB2, e = 0.49;
NY Cep Delta(gamma) = gamma2 - gamma1 = 32 km/s [7412].
OS Cep Very red.
OT Cep Min II 13.3.
OZ Cep Red.
PS Cep In the region of the cluster NGC 7380. SB2 (P = 2.09168d)
PS Cep [5479].
PV Cep In the dark cloud near the diffuse nebula and the cluster
PV Cep NGC 7023. At the apex of the bright variable fan nebula.
PW Cep In the region of the diffuse nebular and the cluster
PW Cep NGC 7023.
QZ Cep The map of surroundings given in [4015] for BV 323 is in
QZ Cep reality the map for BV 324 = QZ Cep. Min II 11.9.
V0338 Cep Min II 9.52.
V0342 Cep B - V = +3.6.
V0344 Cep B - V = +4.4.
V0345 Cep B - V = +5.0.
V0346 Cep B - V = +4.6.
V0347 Cep B - V = +4.5.
V0351 Cep VB A (B 13m, 20", 135deg). P var. Max = 2430615.57 +
V0351 Cep 2.80511d*E (JD2429160 - 34300); Max = 2435749.12 +
V0351 Cep 12.80556d*E (JD2435310 - 40885) [2830]. Since
V0351 Cep JD2442020 - see Table.
V0421 Cep SB, Porb1 = 5.4136d, Porb2 = 225.44d.
V0447 Cep The variability may be due to the fainter (B) component.
V0448 Cep SB, Porb = 7.7320d.
V0453 Cep SB, Porb = 54.723d.
V0454 Cep SB, Porb = 5.6556d.
bet Cep VB A (A 6m, 0.204", 47.2deg, 1977.9; B 7.84m, A2V, 13.6",
bet Cep 250deg). SB1 (Porb = 10.893d) [6486]. P var.
bet Cep Max(Vr) = 2417359.715 + 0.1904795d*E (JD2415750 - 22000);
bet Cep Max(Vr) = 2422203.790 + 0.1904844d*E +
bet Cep 2.9440d*10**(-11)*E**2 + 3.2671d*10**(-17)*E**3
bet Cep (JD2422000 - 42630) [0177]. Elements given in the Table
bet Cep satisfy observations in 1967 - 69.
del Cep VB A (B 13.0m, 20.0", 285deg; C 6.10m - 6.37m, B7IV,
del Cep 41.0", 191deg. P var. Max = 2393659.856 + 5.366438d*E
del Cep (JD2372200 - 96900); Max = 2413960.73 + 5.366386d*E
del Cep (JD2396900 - 2414050); since JD2414050 - see Table.
del Cep All observations in the interval JD2373090 - 45000 are
del Cep well represented also by the elements with a square term:
del Cep Max = 2442756.490 + 5.366270d*E - 7d*6*10**(-9)*E**2
del Cep [8632].
eps Cep VB A (B 9.5m, 127.8", 15deg, 1918).
eps Cep Multiperiodicity: P2 = 0.068073d
eps Cep (A2/2 = 0.0061m), P3 = 0.011823d? (A3/2 = 0.0022m);
eps Cep A1/2 = 0.0079m.
zet Cep Radial velocity varies.
mu Cep VB A (B 12.3m, 19.4", 262deg; C 12.7m, 41", 299deg).
mu Cep There is also the cycle with 4400d duration [8957].
W Cet S5.5/2e.
RR Cet [Fe/H] = -1.26. P var. During JD2417500 - 28820
RR Cet Max = 2417501.444 + 0.55302577d*E; since JD2433180 - see
RR Cet Table. According to [8726], the graph of O - C deviations
RR Cet from the elements given in [3506] is approximately
RR Cet sinusoidal, with Pi = 2600d and the amplitude 0.025d.
RU Cet (k - b)2 = 0.01. Delta(m) var? P var [2455]. Max =
RU Cet 2426964.019 + 0.5863003d*E (JD2426500 - 28430)
RU Cet [0181]; Max = 2434143.056 + 0.5862676d*E
RU Cet (JD2433100 - 35820) [2431]; since JD2435820 - see Table.
RV Cet Delta(S) = 9.
RW Cet Min II 10.5. P var. During JD2426500 - 41000
RW Cet Max = 2426585.503 + 0.9751814d*E [0001]; since
RW Cet JD2441000 - see Table.
RX Cet Delta(S) = 5. P var. Before JD2428500 Max =
RX Cet 2425938.271 + 0.5737100d*E [3506]; since
RX Cet JD2430000 - see Table.
RZ Cet Delta(S) = 6.7. P var. During JD2426585 - 28630
RZ Cet Max = 2426585.448 + 0.510633d*E [3506]; current
RZ Cet elements - see Table.
SS Cet d = 0.025P. P var. Min = 2429321.250 + 2.9739509d*E
SS Cet (JD2427340 - 30700) [2419]; Min = 2430698.160 +
SS Cet 2.973992d*E (JD2429300 - 36650) [3115];
SS Cet since JD2440000 - see Table.
SV Cet Min II 14.9.
TT Cet Min II 11.1.
TU Cet D = 0.043P. Min II 10.9. Min II - Min I = 0.478P.
TU Cet According to [3564], the spectrum is K2.
TV Cet Min II 9.10. DII = 0.03P. Min II - Min I = 0.494P.
TW Cet Min II 11.14. P var. Min I = 2430965.595 +
TW Cet 0.316852d*E (JD2427650 - 31000) [0192]; Min I =
TW Cet 2433611.3121 + 0.316846d*E (JD2433530 - 615)
TW Cet [0001]; since JD2440000 - see Table.
TX Cet B - V: +0.34, +0.37. Min II 11.12.
TY Cet Min II 12.1.
UU Cet (k - b)2 = 0.08. P var. Blazhko effect?
UV Cet VB B (A 12.45m, dM5.5e; a = 2.1", P = 25a).
VV Cet Min II 11.0. EB type is also possible. RR type with twice
VV Cet shorter period is not excluded.
VX Cet d = 0.026P.
VY Cet Min II 11.70.
VZ Cet ADS 1778 B (B 0.61", 122deg; A = omicron Cet).
VZ Cet Small variations are also observed on the time scale of
VZ Cet several hours, with superimposed 10 - 15 minute variations
VZ Cet and rare flares of approximately 2 minute duration
VZ Cet [6492]. A possible white dwarf with an accretion
VZ Cet disc [8926].
WW Cet VR var (P = 0.160d) [4712].
WW Cet Rapid oscillations (~10 min) of brightness are observed
WW Cet [4709].
WZ Cet Min II 11.0.
XY Cet d = 0.02P. Min II 9.34.
YY Cet Min II 9.2.
ZZ Cet 4 stable oscillations are observed simultaneously:
ZZ Cet P1 = 213.132605s, P2 = 212.768427s, P3 = 274.250814s,
ZZ Cet P4 = 274.774562s.
AA Cet ADS 1581 A (B 7.7m vis, SB 2, F5, 8.5", 304deg).
AA Cet Min II 6.7:. dII = 0.065P.
AB Cet ADS 1849 A (B 9.30m, 12", 293deg). SB? (VR var,
AB Cet P = 2.997814d). The period of magnetic variations is
AB Cet 15.9d [8932].
AD Cet ADS 180 A (B 10m, 3", 4deg).
CL Cet Type ELL: is also possible.
EE Cet The variability may be due to the fainter (B) component.
EL Cet SB2.
del Cet Nonlinear term: +2.20d*10**(-11)*E**2.
omi Cet ADS 1778 A (B = VZ Cet, 0.61", 122deg). Maser
omi Cet SiO, OH, H2O.
S Cha VB A (B 9.29m, 23", 134deg).
T Cha Occasionally quasiperiodic light changes are observed with
T Cha periods 3.2323d, 3.4375d, 4.1800d, 3.2436d operating
T Cha during 6 - 26 cycles. IR excess.
Z Cha VB A (B 5.6"). Eclipses: Min =
Z Cha 2440264.68232 + 0.0744992195d*E + 7.88d*10**(-13)*E**2
Z Cha [8938]. D = 0.065P; d = 0.026P. Depth of Min:
Z Cha 1.73m - 2.11m B before the eclipse; 1.38m - 1.97m B after
Z Cha the eclipse. Periodic variations during Min light [7000].
Z Cha Variations with P = 27.7s during a supermaximum [8049].
RS Cha EA/DM. Min II 6.53. One of the components is a pulsating
RS Cha variable of DSCT type. P is in the range from 0.074d
RS Cha to 0.097d [8403]. Delta(M) = 0.01m - 0.03m in the combined
RS Cha light.
RW Cha Min II 14.6.
RY Cha Min II 14.0.
RZ Cha Min II 8.8. DII = 0.11P.
SY Cha Quasiperiodic variations were observed. (P = 6.2d [4305],
SY Cha P = 7.6d [8946]).
TW Cha Quasiperiodic variations (P = 8.68d [4462]).
VW Cha IR excess.
VZ Cha Quasiperiodic variations (P = 7.27d).
YZ Cha Delta(m) (Min II) = 0.4m.
CG Cha Min II 14.4.
CH Cha Min II 15.1.
CX Cha Min II 15.5. Uncertain elements.
CY Cha Min II 14.0.
CZ Cha Min II 14.6.
DD Cha Min II 14.7.
DG Cha Min II 14.5.
zet Cha SB.
S Cir Min II 10.9.
T Cir Min II 9.4.
U Cir P var. Before JD2417000 Max = 2412560 + 151d*E.
V Cir Min II 11.0. According to [0210], varies in the range
V Cir 10.8m - 13.0m pg.
W Cir The coordinates published by the discoverer are wrong,
W Cir actually the star is in Lupus.
TW Cir Min II 13.3.
UY Cir Red.
UZ Cir Epoch of main Max is given. Resembles R Cen.
UZ Cir Max I - Max II = 160d.
VX Cir P var. Before JD2418000 Max = 2414360 + 427d*E.
AQ Cir Possibly EW type with twice longer period.
AR Cir The magnitude in Min light possibly corresponds to an
AR Cir unresolved companion.
AT Cir d = 0.02d:.
AX Cir SB. VB? (6.5m; 6.5m; 0.5", 143deg, 1913).
BD Cir Min II 9.5.
BF Cir Min II 8.9.
BG Cir Min II 10.3.
BN Cir Deep Min II. Twice shorter period is not excluded.
BR Cir Cir X-1. According to [8951], the object does not coincide
BR Cir with the star (B = 22.5m) labelled as L in the chart in
BR Cir [2911] but is situated in ~1" to the south of it and has
BR Cir M > 23.5m on IIIa-J plates. Gradual increase of X-ray
BR Cir intensity is periodically stopped by an abrupt intensity
BR Cir fall. The moments of such transitions T are represented by
BR Cir the elements T = 2443292.118 + 16.595d*E [2926]. The X-ray
BR Cir intensity falls are accompanied by IR and radio bursts.
BR Cir Vr (e alpha) = +250 km/s. In 25' from the supernova
BR Cir remnant G 321.9-0.3.
tet Cir VB (6.2m, 6.2m, 0.1", 96deg).
T Col SiO maser.
U Col Min II 10.5.
Y Col V2 (NGC 1851).
Z Col V1 (NGC 1851).
RS Col Min II 9.97. dII = 0.021P.
RY Col (k - b)2 = 0.10. P var; nonlinear term: -3.38*10**(9)E**2.
RZ Col Min II 11.20.
VW Col Variability may be due to component B.
TV Col 2A 0526 - 328. VB A (B 15.79m, 10", 330deg). Epoch of Max
TV Col of short-term photometric variations is given. The
TV Col following elements describe, respectively, moments of Max
TV Col Vr for Balmer lines and moments of Max for the
TV Col comparatively long-term photometric variations which are
TV Col due to the beat phenomenon for the photometric and
TV Col spectral periods: Max Vr = 2444227.631 + 0.228600d*E;
TV Col Max = 2444191.5 + 4.024d*E. Flickering up to 0.15m B and
TV Col flares up to 0.3m U are also observed [8960].
R Com OH emission.
S Com Delta(S) = 8.
T Com OH, H2O emission.
U Com Delta(S) = 5.
V Com P var. Max = 2424518.219 + 0.46913844d*E
V Com (JD2420900 - 26900) [0218]; since JD2438100 - see Table.
V Com Delta(S) = 8.
W Com Radio source ON 231.
X Com Z = 0.092. Spectrum description [7415, 8966].
Y Com In the region of the globular cluster M 53 (NGC 5024).
Z Com In the region of the globular cluster M 53 (NGC 5024).
RR Com In the region of the globular cluster M 53 (NGC 5024).
RS Com In the region of the globular cluster NGC 5053.
RT Com In the region of the globular cluster NGC 5053. A var;
RT Com P var. Max = 2423113.496 + 0.5651925d*E (JD2422700 -
RT Com 26450) [0222]; since JD2438535 - see Table.
RU Com In the region of the globular cluster M 53 (NGC 5024).
RV Com In the region of the globular cluster M 53 (NGC 5024).
RW Com In the region of the Comae Berenices cluster. dI = 0.04P;
RW Com Min II 11.56. P var.
RW Com Min I = 2433040.406 + 0.23734705d*E (JD2419680 - 34550)
RW Com [0185]; since JD2439600 - see Table.
RY Com P var. Max = 2425007.450 + 0.46894835d*E (JD2425000 -
RY Com 27500) [3506]; Max = 2432674.390 + 0.4689397d*E
RY Com (JD2432600 - 38110) [3415]; since JD2438100 - see Table.
RY Com (k - b)2 = 0.07.
RZ Com Possible member of the Comae Berenices cluster. Min II
RZ Com 11.09; dI = 0.043P, dII = 0.039P. P var.
RZ Com Min I = 2433396.737 + 0.33850556d*E (JD2425000 - 33300)
RZ Com [0226]; since JD2433300 - see Table.
RZ Com Shape of the light curve varies.
SS Com Min II 11.9.
ST Com Delta(S) = 10.
SX Com In the region of the globular cluster NGC 4147.
SZ Com In the region of the globular cluster NGC 4147.
TU Com Shape of the light curve, A and P vary. Mean elements
TU Com are given in the Table. Possible period of Blazhko effect
TU Com is 75d [3584]. [Fe/H] = -1.43.
UU Com Member of the Comae Berenices cluster. Light variations
UU Com are due to rotation and pulsations of the star. Rotational
UU Com period is 2.1953d or 1.0256d or 0.9178d. Period of
UU Com pulsations is 0.0227d (A ~0.01m). According to [7985]
UU Com there are two periods of pulsations: P1 = 0.0274d and
UU Com P2 = 0.0209d
UU Com (P2/P1 = 0.76).
UV Com [Fe/H] = -1.44.
UW Com [Fe/H] = -1.22.
UX Com Min II 10.13. P var; nonlinear term: -3.75d*10**(-8)*E**2.
UY Com [Fe/H] = -1.51.
UZ Com [Fe/H] = -1.44.
VV Com [Fe/H] = -1.53.
VW Com VB (12.00m, dM 3.5e; 12.3m, dM 4e, 3.0", 23deg, 1945).
VW Com Range of total brightness variation
VW Com is given. According to [8363] the component B is
VW Com variable. However both components may be variables.
VY Com Min II 14.5.
AI Com Member of the Comae Berenices cluster. VB A (B 6.63m,
AI Com 145", 251deg). Pulsations are possible: P = 0.052d
AI Com (A = 0.02m) [8975].
AL Com Within 8' to the south-east from the nucleus of M 88
AL Com (NGC 4501) galaxy.
AQ Com Min II 15.7.
BM Com Min II 13.8.
BS Com P var. Max = 2434453.31 + 0.36341d*E (JD2434130 - 35230);
BS Com since JD2435590 - see Table. Shape of the light curve
BS Com varies.
BZ Com [Fe/H] = -1.21.
CC Com In the region of the Comae Berenices cluster. Min II
CC Com 12.09; dI = 0.03P.
CD Com [Fe/H] = -1.78.
CF Com Shape of the light curve varies.
CG Com [Fe/H] = -1.06.
CI Com RRC?
CK Com P var. Max = 2437370.71 + 0.6940159d*E (JD2437370 - 40130);
CK Com Max = 2441630.35 + 0.6939080d*E (JD2440130 - 41630);
CK Com since JD2441630 - see Table. Blazhko effect.
CK Com [Fe/H] = -1.68.
CL Com [Fe/H] = -1.00.
CN Com Min II 13.5.
CP Com [Fe/H] = -1.19.
CT Com In the region of the Comae Berenices cluster.
CV Com In the region of the Comae Berenices cluster.
CX Com In the region of the Comae Berenices cluster. Not member
CX Com of the cluster.
DD Com Min II 14.90.
DG Com Min II 14.6.
DL Com P var?
DR Com EW? P = 0.45184d?
DS Com [Fe/H] = -1.32.
DT Com [Fe/H] = -1.60.
DU Com [Fe/H] = -1.45.
DV Com [Fe/H] = -1.57.
DW Com [Fe/H] = -1.53.
EE Com P = 0.539533d also satisfies observations. [Fe/H] = -1.64.
EF Com [Fe/H] = -1.90.
EG Com [Fe/H] = -1.29.
EI Com [Fe/H] = -1.68.
EL Com P = 0.52362d also satisfies observations.
EM Com [Fe/H] = -1.64.
EN Com [Fe/H] = -1.19.
EO Com [Fe/H] = -1.51.
EP Com [Fe/H] = -0.98.
EQ Com Min II 15.3.
ER Com [Fe/H] = -1.51.
ES Com [Fe/H] = -2.02.
EW Com [Fe/H] = -1.77.
EX Com P = 0.558359d? [Fe/H] = -1.48.
EY Com Min II 18.0.
EZ Com P = 0.568349d? [Fe/H] = -1.16.
FG Com P = 0.3098d also satisfies observations.
FK Com Wide emission lines, Halpha and H, K CaII, of variable
FK Com intensity. Epoch of light minimum is given.
FM Com The member of the Comae Berenices cluster. Multiperiodicity.
FM Com Cycle of 0.0713d was observed also [8989].
FO Com In the region of the Comae Berenices cluster.
FP Com In the region of the Comae Berenices cluster. mu = 0.23",
FP Com P = 158deg. Red.
FZ Com P = 4.704864d?
GM Com In the region of the Comae Berenices cluster.
GN Com Member of the Comae Berenices cluster. P > 1d.
GO Com In the region of the Comae Berenices cluster.
GP Com mu = 0.38", p = 286deg. SB (Porb = 0.032306d).
GP Com Unique object G 61-29. Consists of two interacting white
GP Com dwarfs. The lower mass star, a helium white dwarf,
GP Com transfers mass to the higher mass star surrounded by an
GP Com accretion disk. Usually flares are being observed with an
GP Com amplitude about 0.2m V, 0.5m U lasting about 20 seconds
GP Com [7417, 8991]. Sometimes periods of photometric activity
GP Com arise when amplitude of light variations reaches 0.6m V
GP Com and sharp passages from maxima to minima are being
GP Com observed; the duration of these minima reaches up to 0.14d
GP Com [7417]. When the star is most active, periodic light
GP Com oscillations appear with P = 105 seconds and amplitude
GP Com 0.05m - 0.10m V [7062].
GQ Com Z = 0.165. Emission H, [OIII]. Irregular light variations.
GQ Com = +0.16.
HH Com Epoch of Min in V system is given.
HI Com In the region of the Comae Berenices cluster.
HK Com In the region of the Comae Berenices cluster.
HM Com In the region of the Comae Berenices cluster.
HN Com In the region of the Comae Berenices cluster.
HO Com In the region of the Comae Berenices cluster.
HP Com In the region of the Comae Berenices cluster.
HQ Com In the region of the Comae Berenices cluster.
HR Com In the region of the Comae Berenices cluster.
HS Com In the region of the Comae Berenices cluster.
HT Com In the region of the Comae Berenices cluster.
HU Com In the region of the Comae Berenices cluster.
HV Com In the region of the Comae Berenices cluster.
HW Com In the region of the Comae Berenices cluster.
R CrA In the head of the bright cometary nebula NGC 6729.
R CrA IR excess.
S CrA VB A (B 13.5m, 1", 137deg). IR excess.
T CrA In the bright cometary nebula NGC 6729. IR excess.
V CrA Quasiperiodic variations (P ~75d, Delta(V) ~ 0.2m - 0.9m).
V CrA IR excess.
RS CrA sp of two close stars; each of them or both may be
RS CrA identified with CoD -39deg 13082.
RW CrA Min II 9.4.
SS CrA V1 (NGC 6541).
SV CrA The period may be twice shorter.
TY CrA VB A (B 13.3m, 4", 138deg; C 58", 24deg).
TY CrA In the bright nebula NGC 6726/27. P = 1.92d is not
TY CrA excluded, in that case Min II = Min I. On the basis of
TY CrA visual observations 8.7 - 12.4 v (presumably "spurious
TY CrA variability" due to the difficulties of estimates over
TY CrA the bright background of the nebula), and the star
TY CrA was classified as INSA.
TZ CrA Min II 9.72.
UU CrA Min II 11.0.
UX CrA The period may be twice shorter.
UY CrA P var?
VV CrA In the region of the bright nebula NGC 6729. IR excess.
AF CrA P var. Before JD2418060 Max = 2413710 + 483d*E; since
AF CrA JD2418060 - see Table.
AL CrA B - V: +0.65, +1.30. [A/H] = -0.2.
AN CrA P var. Nonlinear term: -0.006d*10**(-6)*E**2.
AU CrA P var. Nonlinear term: -0.026d*10**(-6)*E**2.
AY CrA Min II 15.2.
BG CrA Min II 15.1.
BH CrA P var. Nonlinear term: -0.023d*10**(-6)*E**2.
CM CrA P var. Nonlinear term: -0.007d*10**(-6)*E**2.
CR CrA Min II 15.7.
CS CrA Min II 15.2.
CY CrA P var. Nonlinear term: -0.002d*10**(-6)*E**2.
DG CrA In the region of the bright nebula NGC 6729. IR excess.
DL CrA Min II 13.6.
DN CrA P var. Nonlinear term: +0.006d*10**(-6)*E**2.
DZ CrA d = 0.02P.
EE CrA var, 13.5m - 15.5m, P2 = 3000d - 5000d
EE CrA Delta(m) (P1 = 167d) ~1.5m.
EK CrA P var. Before JD2422600 Max = 2411870 + 421d*E.
FF CrA Before JD2423000 Max = 2411530 + 140.2d*E.
FK CrA Min II 14.5.
FS CrA Min II 14.5.
FW CrA Before JD2416600 Max = 2411190 + 112.2d*E.
GS CrA Before JD2422600 Max = 2414070 + 284d*E.
IT CrA Min II 13.6.
KQ CrA [A/H] = -0.7. B - V: +0.76, +1.23.
KT CrA Red.
LU CrA P = 182d is possible.
MS CrA Yellow.
MT CrA Min II 13.1.
NO CrA Reddish.
QR CrA Reddish.
V0347 CrA B - V: +0.82, +1.17.
V0350 CrA Min II 13.4.
V0385 CrA The period may be spurious.
V0413 CrA (k - b)2 = 0.11.
V0428 CrA The period may be twice shorter.
V0449 CrA [A/H] = -0.3.
V0454 CrA Min II 10.5.
V0455 CrA d = 0.05P. Min II 13.7.
V0457 CrA Epoch of Min is given. EW type is also possible, in that
V0457 CrA case the value of P should be doubled.
V0465 CrA Min II 14.2.
V0467 CrA P var?
V0471 CrA Min II 13.3.
V0478 CrA Sometimes a cycle 60d - 70d.
V0480 CrA Min II 13.9.
V0490 CrA P var? The elements represent the observations of 1944.
V0493 CrA P var?
V0501 CrA Min II 13.4. Twice shorter period is possible.
V0503 CrA d = 0.03P.
V0511 CrA Twice longer period is possible.
V0512 CrA P var?
V0513 CrA Min II 13.2.
V0514 CrA Min II 14.0.
V0527 CrA P var.
V0535 CrA P var.
V0541 CrA P var?
V0545 CrA VB. Combined brightness with a faint companion is given.
V0553 CrA P var?
V0566 CrA Min II 12.7.
V0568 CrA Sometimes a cycle 60d - 80d.
V0569 CrA Min II 13.1. EB type is possible.
V0571 CrA Min II 14.7.
V0572 CrA Min II 14.0.
V0577 CrA Min II 13.2. RR type with twice shorter period is possible.
V0578 CrA RV type with P = 118d is possible.
V0580 CrA Min II 14.4.
V0595 CrA P var.
V0601 CrA Epoch of min is given.
V0603 CrA Slightly noticeable Min II at the phase 0.5P.
V0604 CrA d = 0.03P.
V0607 CrA Min II 14.3.
V0612 CrA d = 0.03P.
V0615 CrA P var?
V0622 CrA Sometimes 55d - 60d cycles.
V0633 CrA P var.
V0634 CrA Min II 13.9.
V0648 CrA Min II is felt at the phase 0.5P.
V0659 CrA P = 189.4d is possible.
V0667 CrA In the region of the bright cometary nebula NGC 6729.
V0667 CrA The spectral type is earlier than K.
V0676 CrA RR type is possible.
V0686 CrA Max I 5.34, Min I 5.41, Max II 5.35, Min II 5.40 [8970].
V0691 CrA 4U 1822-37. Emissions CIII/NIII lambda 4640 - 50,
V0691 CrA He II lambda 4686, CIV lambda 1550 etc.
V0692 CrA P = 0.83d is possible.
eps CrA Min II 4.95.
R CrB IR excess.
S CrB OH, H2O, SiO maser.
T CrB VB? A (B <= 12m, 0.2"). SB (P = 227.6d).
T CrB The spectral period is present in the photometric data of
T CrB 1891 - 1917 and 1960 - 1971 [8978]. The epoch of the first
T CrB outburst JD2402734 (1866). Two smaller outbursts were
T CrB observed in UV light, JD2438030 (1963) and 2442543
T CrB (1975) [8979].
U CrB Min II 7.72. P var.
RR CrB P2 = 377d. Delta(m) (P1) ~0.5m, Delta(m) (P2) ~0.6m.
RS CrB P2 = 69.5d [1100]. Main period oscillation: 9.1m - 11.6m.
RT CrB Nonlinear term: +2.01d*10**(-8)*E**2. Min II 10.52 (var).
RT CrB DII = 0.09P.
RV CrB P var. Max = 2428285.608 + 0.3316217d*E (JD2428285 - 31610);
RV CrB Max = 2431705.349 + 0.3317313d*E
RV CrB (JD2431705 - 32954); Max = 2433030.572 + 0.331705d*E
RV CrB (JD2433030 - 36814) [5496]; Max =
RV CrB 2440001.453 + 0.331569d*E (1967 - 1971) [6237];
RV CrB Max = 2441451.413 + 0.331619d*E (1972 - 1974)
RV CrB [7032]. The Table gives current elements. On
RV CrB the period changes see also [3506]. Blazhko effect?
RW CrB d = 0.028P. Min II 10.29.
TW CrB Min II 11.0.
TZ CrB ADS 9979 A (B 6.72m, GIV, 6.6", 233deg, 1980).
TZ CrB SB2 (P = 1.139789d).
TZ CrB Epoch of Min is given. The variation presented in the
TZ CrB Table is superimposed by a second one, with the same
TZ CrB amplitude and P = 0.1d. The amplitude is given
TZ CrB for the combined light of ADS 9979 A and B, the
TZ CrB mean magnitude is for ADS 9979 A.
UU CrB During JD2444381.73 - .76 a slow flare was observed, with
UU CrB maximal amplitude 0.30m in the IK band and 0.18m in the
UU CrB U band.
alf CrB lambda eff = 7230 A: DI = 0.034P, DII = 0.018P,
alf CrB Min II - Min I = 0.66P, depth of Min I 0.10m, Min II
alf CrB 0.025m.
bet CrB VB A (B ~ 5m - 6m, 0.2", ~130deg, 1978). SB (P = 3833.7d).
bet CrB Magnetic field var, P = 18.487d. The epoch of Min light
bet CrB is given.
gam CrB ADS 9757 (4.2m, 5.6m; A = 0.74", P = 91.0a).
U Crv VB A (B 13.5m, 0.4' p).
W Crv Min II 11.86. The light curve is asymmetrical, the maxima
W Crv differ in hight by 0.10m.
Y Crv Min II 11.7. RRC type with twice shorter period
Y Crv is possible.
Z Crv d = 0.06P.
RV Crv Elements do
RV Crv not satisfy some of the published moments of Min.
RZ Crv Min II 13.9.
SX Crv Min II 9.23. The shape of the light curve varies. Depth of
SX Crv Min I 0.20m, depth of Min II 0.18m. In 1972 the system
SX Crv became fainter than in 1971 by 0.06m.
TY Crv SB2.
R Crt Periods of light constancy which last up to 250d occur
R Crt every two or there thousand days. OH, H2O maser.
S Crt H2O maser.
T Crt Mean light var, P2 = 1006d.
V Crt Min II 10.1; Min II - Min I = 0.57P.
W Crt (k - b)2 = +0.21.
X Crt (k - b)2 = +0.02.
Z Crt d = 0.016P.
RR Crt P = 293d or 146d is possible.
RV Crt Min II 9.4:.
SU Crt [Fe/H] > -0.3.
SV Crt ADS 8115 A (B 11.5m vis, 1", 220deg). SB2 (P = 5.90513d,
SV Crt apsidal motion, P ~700a). Epoch of Min I in B light is
SV Crt given. Depth of Min II is 0.015m. EuII and SrII in
SV Crt emission.
R Cru In the region of the open cluster NGC 4349.
T Cru In the region of the open cluster NGC 4349.
U Cru P var. Max = 2410143 + 351.4d*E (JD2410100 - 14100) [0237];
U Cru since JD2437600 - see Table.
W Cru Min II 9.3.
SU Cru [A/H] = -0.8.
SV Cru In the region of the open cluster Ruprecht 97.
SV Cru Non-member of the cluster.
SW Cru VB A (B 14.0m, 12"). (k - b)2 = 0.27.
SY Cru d = 0.05P?
TU Cru Min II 11.5.
TW Cru Min II 12.85:.
TX Cru It is not excluded that actually P is much shorter,
TX Cru close to 1d, for instance.
TZ Cru P = 2.091140d?
UW Cru Min II 12.9; Min II - Min I = 0.536P.
UX Cru VB A (B 10"). Min II 12.4; Min I - Min II = 0.325P;
UX Cru DII = 0.025P.
VY Cru Min II 13.5.
VZ Cru P = 1.125810d?
WW Cru Min II 13.0.
WX Cru d = 0.040P. Light variability in maximum is noted.
WY Cru VB A. P = 9.013290d?
XX Cru P = 3.28566d?
XY Cru Min II 11.7.
XZ Cru P = 1.6495930d?
YY Cru Min II 13.0.
YZ Cru Min II 13.1.
ZZ Cru Min II 9.8.
AB Cru Min II 8.9.
AC Cru Min II 12.1.
AD Cru VB A (B 14.5m, 10", 270deg). P var. Max = 2434918.160 +
AD Cru 6.39844d*E (JD2423800 - 35400) [2309];
AD Cru since JD2441000 - see Table.
AE Cru Depth of Min II 0.03m.
AF Cru According to [1122] Algol-type with the elements:
AF Cru Min I = 2424988.959 + 1.895669d*E, D = 0.06P.
AF Cru This conclusion must be checked. The star deserves careful
AF Cru investigation.
AG Cru The blue component is possible [9004].
AI Cru In the region
AI Cru of the open cluster NGC 4103. Min II 9.94.
AQ Cru Min II 13.8.
AT Cru Min II 12.6.
AW Cru Min II 13.9.
AY Cru Min II 11.2.
BB Cru Min II 14.0.
BC Cru Depth of Min II 0.03m.
BD Cru Depth of Min II 0.05m.
BF Cru Min II 12.3.
BH Cru Epoch of Min I is given in the Table. The light
BH Cru curve like the light curves of R Cen and R Nor
BH Cru has two maxima and two minima of different
BH Cru depths. Max I 7.6m (0.22P), Min II 8.0m (0.41P),
BH Cru Max II 7.2m (0.53P).
BI Cru Spectrum description [4949].
BK Cru In Coalsack region.
BM Cru In Coalsack region.
BP Cru 3U 1223-62. A unique X-system. Consists of an X-pulsar
BP Cru with pulse period 698s [9018] moving on an excentric
BP Cru orbit (E = 0.47) around the ellipsoidal B2 supergiant with
BP Cru orbital period of 41.51d. Accretion of the stellar wind
BP Cru from the primary star on the pulsar increases during the
BP Cru periastron passage. Therefore large X-flares are observed
BP Cru with the elements: T (X Max) = 2433158.09 + 41.51d*E.
BP Cru Optical flares are possible.
BQ Cru B - V: +1.13, +0.88.
BS Cru In the open cluster NGC 4755.
BT Cru In the open cluster NGC 4755.
BU Cru In the open cluster NGC 4755.
BV Cru In the open cluster NGC 4755.
BW Cru In the open cluster NGC 4755.
DU Cru The identification with NSV 06012 (SIMBAD) is wrong.
bet Cru VB A (B 11.4m, 44.3", 322deg; C 7.5m, 372", 23deg).
bet Cru Interferometric binary. Multiple periods (the total V
bet Cru amplitudes of corresponding oscillations are indicated
bet Cru in brackets): P0 = 0.2365072d (0.034m), P1 = 0.160466d
bet Cru (0.029m), P2 = 0.121383d (0.01m), P02 = 0.249373d
bet Cru (0.016m), P13 = 0.24273d (0.024m), P24 = 0.23931d
bet Cru (0.028m), P03 = 0.16342d (0.016m), P14 = 0.16171d
bet Cru (0.029m).
tet 2 Cru SB (P = 3.4380d). BCEPS, P > 1h? [8420].
lam Cru Type ELL with
lam Cru P = 0.7902d is possible. Amplitude and shape of
lam Cru the light curve vary. The secondary oscillation
lam Cru (A = 0.007m) with the elements Max = 2441779.034 +
lam Cru 0.1793d*E is possible.