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 by outbursts up to 4m with intervals of 10 - 20 years. In the intervals cyclic variations are observed with the mean period of 632d and variations with cycles of several days and Delta(m) ~ 0.1m - 0.5m. The spectrum is symbiotic, with features of a late M giant, narrow low-excitation emission lines (Bleq) and forbidden lines 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. Nonlinear term: -6.33*10**(-11)*E**2. During JD2433477 - 43878 linear elements are satisfactory: Min = 2441141.8888 + 0.62892984d*E. Period changes according to a sine law are possible [08002]. RU And P var. Max = 2419857 + 243.0d*E (JD2412800 - 20000); Max = 2434551 + 233.24d*E (JD2420000 - 34550). Since JD2435000 - see Table. Delta(m) ~ 4m - 5m (before JD2429600), ~1m (JD2429600 ~ 33600), up to 3m (JD ~2436000), ~1.5m (JD ~2436700). In 1970 - 1972 showed quite irregular variations. RX And SB (P = 0.21173d). Cyclic variations with P ~ 38s - 54s were observed after a normal maximum; after a short maximum no periodicity was found [08004]. SS And Two long period variations are also observed: P = 650d, P = 3800d. ST And P var. Max = 2418370 + 337.3d*E (JD2418000 - 28000). Since JD2428000 - see Table. SU And VB A (B 12.77m V, F0V:, 15"). SV And The magnitude in Max varies periodically, P = 930d, P = 5400d? [02146]. SW And [Fe/H] = +0.16. P var. Nonlinear term: -1.229d*10**(-10)*E**2 [01959]. Since 1959 Max = 2436466.828 + 0.442270121d*E [06929]. The shape of the light curve varies with Pi ~36.83d = 83.28 P. The deviations (O - C) satisfy the elements of Blazhko effect Max(O - C) = 2436816.23 + 36.921d*N. Secular trend and cyclic (P ~2a) variations of (O - C) are possible [08005]. SY And d = 0.027P. TT And Min II 11.6? TU And P var (Pi ~37a?). TV And P var? Delta(m) strongly varies. TW And d = 0.020P. Min II 8.94. P var. Min = 2428845.422 + 4.122739d*E (JD2420050 - 32000). Since JD2432000 - see Table. TZ And P1 = 118d: [00882]. Mean magnitude varies with P2 = 974d [00098]. P = 135d (JD2437545 - 38377) [03367]. UU And P var. Min = 2428832.536 + 1.486311d*E (JD2421455 - 23740) [02262]; Min = 2428832.465 + 1.48629d*E (JD2428830 - 35012) [00745]. Since JD2441100 - see Table. UW And P var. Before JD2430000 Max = 2418585 + 236.7d*E. Since JD2436000 - see Table. WW And d = 0.012P. WX And P var. Max = 2422613.614 + 3.0012544d*E (JD2422610 - 34712) [01240]. The Table gives current elements. d = 0.03P in 1972 and probably varies. WZ And Min II 11.9. P var [02262]. Min = 2435075.342 + 0.695662d*E (before JD2440500); probably Min = 2440872.290 + 0.6956576d*E since JD2440500. The elements in the Table represent all the observations satisfactorily. XX And P var. Max = 2418001.938 + 0.7227486d*E (1908 - 1932); Max = 2427106.403 + 0.7227591d*E (1932 - 1946) [02264]. Since 1946 - see Table. Delta(S) = 9. Blazhko effect: Max = 2437578 + 36d*N [03111]. XY And Blazhko effect is possible. XZ And Min II 10.16; DII = 0.26P. P var [02431, 06932, 08008, 08593]. Min = 2432883.6046 + 1.3572708d*E (JD2431700 - 36150) [01977]; Min = 2441954.340 + 1.357293d*E (since JD2436200). The elements in the Table represent all the observations satisfactorily. AA And Min II 10.5. AB And Min II 10.20. P var. Period increased suddenly in 1953 ( ~JD2434500); no period changes later [02509, 05222]. Elements since 1953 - see Table. AC And Unusual multiperiodical variable. Second oscillation: Max = 2432467.373 + 0.71124243d*E; P3 = 0.421069d [08187], see also [08294, 08295]. Delta(S) = -1:. AD And Min II 11.6. Depth of minima in yellow light: 0.62m (Min I), 0.58m (Min II) [03141]. Min II - Min I = 0.494P. P var. Min = 2428718.402 + 0.9861940d*E (JD2417460 - 29640) [01983]. Since JD2428700 - see Table. AE And In the M31 galaxy. Strong UV continuum. Emissions: H, He I, Fe II, [Fe II]. AF And In the M31 galaxy. Strong UV continuum. Emissions: H, He I, Fe II, [Fe II]. AG And According to [08296], DSCT:, Min = 2442636.5868 + 0.0347d*E, A = 0.5m. AM And VB A (B 0.25' S). AN And Min II 6.09. The existence of the third body in the system is possible. Sp(Met) = F2 - F5. AP And Min II 11.9. The period may be 2 times shorter. AT And B - V: +0.42, +0.56. Delta(S) = 3. See [08299] for data on period variations and a detailed study. BD And Min II 11.4. BE And Average cycle: 137d [01993, 02267]; 156.8d after JD2431700. BL And Depth of Min II 0.24m: P var? Min I = 2429491.255 + 0.7223779d*E (JD2415800 - 33900) [01995]. Since JD2433900 - see Table. BX And ADS 1671 A (B 9.7m, 20", 59deg). Min II 9.15. Possible period change from 0.61011222d to 0.61011534d (~1952). On the period changes see also [08657]. BY And According to [08658], SRB:. CC And Possibly in a binary with Porb = 10.469d. Delta(m) and the light curve shape vary with a period 5.23714d or 10.469d [08016]. According to [03120], 4 periods are present: P2 = 0.0632083d. First overtone was not found. Other periods are resonances. CG And P var: 3.7430d (1950), 3.7394d (1963) [05224]. Cyclic period changes are possible. According to [06941], short period oscillations (P = 2h 04m) are present. A number of observers do not find short-term variability. CM And According to [00821], Max = 2428380 + 140d*E and Max = 2430616 + 124d*E, and the star resembles UU Her. CN And Min II 9.96. CO And d = 0.06P: CP And d = 0.01P? Depth of Min II 0.05m? CU And d > 0.034P ([06943], according to visual observations.) DI And DCEP? [03165]. 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 [02275]; then P changed abruptly. Delta(m) changes by ~0.3m, Max A1 = 2436078.8 + 69.486d*N1, Max A2 = 2437646.65 + 69.719d*N2. Other possible cycles are 2000d (interaction of cycles N1 and N2) and ~30 years [08019]. DS And In the field of the open cluster NGC 752. Min II 10.7. DZ And According to [04008], type RCB, spectrum R. According to [06945], since 1961 is in Max light all the time. According to [06946], the spectrum is not characteristic of RCB stars. According to [08660], the star was bright near the moments of Min light given in [04008]. EG And P = 40d or 80d [08020]. Absorption spectrum with overlaying emissions of high excitation [04434, 08598]. Strong variable magnetic field [04435]. Long period variations of light are observed. Radial velocities profiles and equivalent widths of lines vary with P = 470d [08596] (SB? [08597]). Possibly is analogous to HM Sge [08598]. EH And IR excess. The presence of a dust envelope is possible. EO And Very red. EP And Min II 12.5. ET And Delta(B) = 0.035m, Delta(U) = 0.07m. The Table gives the epoch of Max light. Observations may be represented by the periods 0.723d and 1.61553d [08022, 07946]. According to [08023], in June - December 1977 Min = 2443337.4725 + 0.49925d*E, other periods are not satisfied by observations. According to [08599], Max(U) = 2439751.28 + 0.617135d*E (1967 - 1971). SB, Max(Vr) = JD2443718.0 + 48.304d*E [08301]. Photometric periods could not be found in radial velocities. EX And Possible Min II 13.0:, Min II - Min I = 0.55P. EY And I - K = 5.38; the presence of a dust envelope is possible [06947]. FF And 10.35m - 10.42m V outside flares; M - m = 0.50P. Porb = 2.170304d [08024]. According to photometric observations, P = 2.14d (1971), P = 2.15d (1972), P = 2.19d (1973) [06948]. FG And According to [04156], EA; Min = 2436074.528 + 0.99772d*E. FL And d = 0.02P. FZ And mu = 1", p = 64deg. GK And Min II 11.5. GN And ADS 409 A (B 13.3m, 2", 6deg; C 11.6m, 141", 130deg). Different authors give spectral types F0 III, F2V, Am (probably based on different criteria). GP And Delta(m) changes with P2 = 0.64d. A wave with P3 = 0.012161d is present. The mean magnitude and the shape of the light curve vary [08302]. GQ And ADS 246 B (A = GX And; B 37", 61deg). B - V = +1.80. X-ray source. GR And Min (magnet.field) = 2442288 + 525d*E. Magnetic field varies (-250 to -1030 Gauss). Period of changes of C1 is near 1.5 years [07893]. According to [06257], period of changes in u is near 1 year or longer. GS And B - V = +1.7 in normal light. GX And ADS 246 A (B = GQ And, 37", 61deg). Delta(U) = 0.55m. SB? (conflicting data). GY And SB1 (P = 273.2d [07324], P = 272.99d [08303]). For spectral changes, variations of light and magnetic field it is possible that P = 23a [07004] or 20.60a [08303]. [08022] gives P ~36.5d and Delta(V) ~0.049m. Periods 4.92a and 1.8d may exist [08303]. GZ And B - V: +0.77, +0.82. ADS 1693 A (B 11.13m, 8", 31deg). Min II 11.58. P var? The period is based only on Minima I [06830] and was improved with account of recent data. HH And Subdwarf? [06581]. mu = 1.82", p = 176deg. HI And B - V = 1.8m outside flares. HN And Max(U) = 2438327.8 + 69.433d*E [08022]. SB (P = 106.27d [07435]). HQ And According to [08659], a probable cataclysmic binary; similarity to AM Her and AN UMa is noted. HR And d = 0.05P. HT And B - V = +0.60. In the region of M 31. HU And Min II 17.2. In the region of M 31. HV And According to [08659], a probable cataclysmic binary; 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 [08659], a probable cataclysmic binary; similarity to AM Her and AN UMa is noted. IP And d = 0.02P:. KK And The light curve has double-wave shape [07740]. Long period variations were found [07955]. KU And I - K = 4.63. SR type is possible. Surrounded with a dust envelope [08029]. 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"). Epoch of Max U light is given. Hbeta index varies in the range of ~0.02m with P ~3h [08030]. Rapid rotation. zet And Depth of Min II 0.1m. SB. Unstable light curve. Most notable variations on the rising branch of Max II [08030]. Many peculiarities in the spectrum. lam And SB1 (P = 20.52d). omi And v sin i = 300 km/s; VB(0.3"; possibly also 0.05" - according to speckle-interferometric data). Shell spectrum appeared and disappeared several times since 1890. Different authors attributed the star to EB type. According to [05955], The changes of light may be explained also by intrinsic variations of a single shell star. They are represented by elements: Min I = 2439470.628 + 1.0185d*E. According to [02572], Min I = 2436174.430 + 1.5998398d*E. The periodogram analysis shows a stable peak at P ~0.84d [08032]. A possible shell event was observed late in 1975. S Ant Min II 6.87. P var? T Ant CWB? P var. [A/H] = -0.0. P = 5.9098d (JD2428187 - 34688), P = 5.8976d (JD2434688 - 37660) [05387]. The Table gives mean elements which satisfy all 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 = 0.57431618d (JD2422070 - 25600); P = 0.57431216d (JD2425600 - 29000) [01113]. (k - b)2 = 0.00. WZ Ant Min II 11.8. XX Ant Min II 9.1. XY Ant Depth of Min II 0.3m - 0.5m pg. XZ Ant Min II 10.2. Z Aps Possibly also an eclipsing binary. RT Aps Strong variations of period and the shape of the light curve [06152]. 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 changes with superimposed variations of eclipsing 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, OII. Variable radio source. SiO maser. The secondary may be an accreting white dwarf. The star is embedded in an expanding gaseous nebula several hundred years old. A cycle ~24a and longer-term variations are possible in the changes of radial velocities and period. U Aqr Strong bands of 12C2, CN, lines of SrII, YII in the spectrum; hydrogen deficiency. A probable halo star (Vr ~100 km/s.). Z Aqr 1969 - 70: P = 100d +- [05973]. RY Aqr P var. Min = 2433872.352 + 1.966598d*E (before JD2428000); Min = 2440824.410 + 1.966620d*E (JD2428000 - 41000); Min = 2440824.410 + 1.966611d*E (JD2441000 - 43800). Since JD2443800 P = 1.966554d? The Table gives elements representing observations after JD2428000 with the accuracy +-0.1d. ST Aqr Min II 9.37. P var. Min = 2423640.271 + 0.78101367d*E (JD2423500 - 26000) [02037]. Since JD2439700 - see Table. SU Aqr ADS 16318 A (B 10.7m, 5", 144deg). Min II 10.5. P var? SV Aqr Cycle 200 - 300d is possible. SW Aqr P var. (k - b)2 = 0.01. SX Aqr P var? Delta(S) = 9. SZ Aqr Epoch of Min is given. TT Aqr VB A (B 15m, 3", 135deg). TZ Aqr Delta(S) = 5. VY Aqr Second outburst: Max ~JD2437897 (1962), ~9m pg [03129]. 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. Small fluctuations of period are possible. AE Aqr Unusual flare X-ray system with pulsar. Becomes bluer in Max. In Min B - V = +0.92. Shows rapid irregular variations, which differ it from UV stars and UG system, though the spectra are somewhat similar. Simultaneous photoelectric and spectroscopic observations [03131] show the existence of two types of flares: 1) intensification of emission lines accompanied by brightening in U and B; 2) intensification of continuum leading to brightening in U, B and V ("white flare"). Detailed spectroscopic investigation [01971]. Porb = 0.41165794d + 1.12*10**(-10)*E, The epoch T0 = JD2439030.621 [08672]. In the X-ray band (0.1 - 4.0 keV) pulsations with P = 33.0767s are observed [08673]. In the optical range pulsations with P0 = 33.076737s as well as with P1 = 16.5s were noted [08674, 08675]. AT Aqr Min II 14.7. AX Aqr P var. Before ~JD2427367 Max = 2425417.60 + 0.388135d*E [03113]. AY Aqr Min II 14.3. BH Aqr P var. Before ~JD2431150 Max = 2426948.411 + 0.5258022d*E [03113]. BI Aqr Min II 13.1. BK Aqr Close companion. BL Aqr Waves from 80 to 125d. Mean magnitude changes with cycles from 480 to 700d in the range of 0.3m - 0.6m. BM Aqr The mean magnitude may vary with P = 500 - 600d. BN Aqr Delta(S) = 4:. P var. Before JD2428964 Max = 2426577.901 + 0.46963401d*E [03113]. According to [05391] Max = 2429395.742 + 0.4696410d*E + 3.3*10**(-10)*E**2 (1898 - 1958). BO Aqr P var? (k - b)2 = 0.01. BQ Aqr d = 0.07P. BR Aqr P var? (k - b)2 = 0.16. BS Aqr Delta(S) = 0. P var? BT Aqr B - V: +0.14, +0.52. P var. Blazhko effect. BV Aqr P var. Blazhko effect with Pi = 11.56d and variations of light in Max up to 0.75A. BW Aqr d = 0.01P. Min II 10.8. Min II - Min I = 0.484P. Jensch [00189] considers the secondary Min to be the main one. BX Aqr d = 0.027P. CD Aqr d = 0.012P. Min II 10.2. CE Aqr According to [02548], no variations were found in visual observations during several months in 1954 - 1958. According to [03138], 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 Minor planet (52) Europa. CW Aqr Min II 10.8. CX Aqr Min II 10.8. Broad hydrogen lines. CY Aqr Delta(S) = 2. P var; abrupt change ~1952. Before JD2434000 Max = 2434308.4314 + 0.061038509d*E. The shape of the light curve probably varies. For M - m different authors give values from 0.23p to 0.40p. Beat phenomenon with P2 = 0.2182d is possible [08060]. 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 [08061] variations were noted with Delta(m) ~0.1m and P < 3h, presumably of DSCT type nature. Some sources give A3 for the spectral type. Shell spectrum was observed in May, 1975. Spectral lines were filled with emission and therefore weak, strong absorption in H and K CaII lines was present. Shell effects were not present in the spectra taken in 1971 - 1973 [08062]. DX Aqr VB B (A 7.0m, K0III; B 3.7", 244deg). SB1. d ~0.015P. Depth of Min II ~0.3m. The range of combined brightness is given. DY Aqr d = 0.04P. EE Aqr Min II 8.48. EK Aqr Min II 11.23. EL Aqr P = 0.6345d is possible. EM Aqr According to [06204] P = 0.068d. Period and amplitude vary on very short time scale. Light and colour vary approximately in phase. The beat period, if exists, is shorter than 1d. ET Aqr Period is given according to [08336]. EW Aqr Delta(m) varies. FF Aqr d = 0.059P. SB1. The unique eclipsing system of a red star and probably a blue hot subdwarf. The amplitude of the eclipse is 0.15V, 0.4B, 1.2U. The magnitude in Max varies by 0.35V, 0.33B, 0.22U. Variable shape of light curve. Strong emissions H and K CaII, Halpha in the spectrum. FI Aqr Possibly P = 4.659d or 4.719d. Epoch of min is given. FK Aqr BDS 11854 A (B = FL Aqr, 11.45m, 24", 352deg, 1966). mu alpha = +0.455", mu delta = -0.067". SB2 (P = 4.08322d [00313]). Flares Delta(U) = 0.7 [00344]. 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 in 1957 - 1975, the star became redder. Balmer continuum in emission. Rapid changes in emission lines and in polarization. Existence of a disk or a shell is possible. R Aql P var. Max = 2440038 + 297d*E (JD2427850 - 40000). Since JD2440000 - see Table. For the whole observed period Max = 2399190 + 346.932d*n - 0.239303d*n**2; Pn = 348.980d - 0.554202d*n + 0.000552309d*n**2 [03143]. H2O, OH and SiO maser. Radiobursts. U Aql B - V: +0.84, +1.24. P var. ADS 12503 A (B 14.00m, 35", 349deg, 1900; one more companion 11.7m V, 2", 230deg, 1934). W Aql S 6/6e. Composite spectrum near Min light; a companion (F5 - F8) may exist [03502]. 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 [02392]. Before JD2420260 P = 17.1359d. Current elements - see Table. TT Aql B - V: +0.96, +1.62. P var. [02392]. Before JD2418035 P = 13.7518d. Current elements - see Table. TV Aql P var (changed at ~JD2430000). Before JD2430000 Max = 2429730 + 237.9d*E. TW Aql Cycles 65d or 95d are observed during different time intervals [08714]. UU Aql Mean cycle: 71.3d [04063]; 56d [03144]. UY Aql Cyclic changes of light (P ~400d) with superimposed very rapid variations are noted in [00504]. VX Aql SC5-/8e. According to [04231], the variable is irregular. Lithium star. VZ Aql B - V: +0.61, +1.01. XZ Aql P var. Min = 2424449.277 + 2.139147d*E (JD2424380 - 2430300). Since JD2433000 - see Table. YZ Aql d = 0.03P. P var. AA Aql Delta(S) = 1.0. AC Aql P var. AD Aql CN bands are observed in the spectrum. According to [06928], the range is 8.83 - 13.42 V. AE Aql VB A (B 16.6m, 12", 330deg; C 16.9m, 11", 0deg). The combined light of A, B, C varies in the range 13.9 - 15.8. AF Aql The period may be two times shorter. AL Aql d = 0.04P. AU Aql According to [03146], P = 190d or 380d. BL Aql P var. Max = 2418538 + 159.65d*E (JD2418529 - 29075). During JD2436420 - 38940 - see Table. BY Aql P var? CD Aql Close companion? CL Aql Sometimes maxima predicted according to the elements do not occur. CM Aql Symbiotic spectrum similar to that of Z And [03149]. CR Aql Considerable Blazhko effect is possible. CS Aql Close companion? CT Aql According to [06004], only slow irregular variations with Delta(m) ~0.6 were observed in 1963 - 1968. CU Aql P var? (Possible change ~JD2423000). Earlier Max = 2418591 + 203.7d*E. CV Aql P var? CW Aql Close companion? DD Aql Close companion? DT Aql P var (Change ~JD2425000). Earlier Max = 2423964 + 290.5d*E. DY Aql P var [06107]. EV Aql P var. Before JD2423900 P = 38.67d. [A/H] = -0.3. EX Aql P = 117d is also observed. EZ Aql P var [06107]. 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 physical pair with FH Aql (rho ~20"). According to [00504], the mean cycle of light variations is 3.5d. The level of mean light varies. FH Aql At the edge of the dark nebula Barnard 130. May be a physical pair with FG Aql (rho ~ 20"). According to [00504], 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 [00504]. GU Aql d = 0.02P. GV Aql Nova-like star according to [02089]. GY Aql Maser OH, SiO. HK Aql Type ISB is not excluded. HL Aql P var? The 15m star shown in the charts [02274, 06996] with co-ordinates coincident with those given at the discovery is constant according to [02274]. 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 + 2.863859d*E (JD2426250 - 33000) [02462]; Min = 2433888.366 + 2.863954d*E (JD2433000 - 39000). current elements - see Table. KP Aql Min II 10.43; Min II - Min I = 0.50P; DII = DI. KV Aql During JD2429130 - 31370 - see Table. During JD2428308 - 28433 the star was faint. Max 2436015 also is not satisfied by the elements. LU Aql In [03158] P = 102d is given, and the existence of the variation of mean magnitude with P ~1080d and Delta(m) = 0.4m was suspected. MV Aql Close component, the range is given for combined light. NN Aql Cyclic P variations? NV Aql Variations of mean light with P ~ 900d - 1000d and Delta(m) ~0.6m. OO Aql Min II 9.8. P var. Min I = 2426892.0582 + 0.5067954d*E (1932 - 1934), Min I = 2433925.3762 + 0.5067943d*E [08072]. Since JD2438000 - see Table. The shape of the light curve varies. OX Aql Var 2 in the chart for OW Aql. PP Aql [A/H] = -0.0. CWA type is not excluded. According to [03161] P var. Max = 2415229.15 + 24.0147d*E (JD2415228 - 21064), Max = 2426576.14 + 24.074d*E (JD2426576 - 29489). After JD2432040 Max = 2433141.78 + 23.994d*E. Current elements Max = 2436836.04 + 23.973d*E. PZ Aql P var? According to [05387], before JD2428075 P = 8.7555d; P = 8.7504d (JD2428075 - 34725); since JD2434725 P = 8.7573d. See also [02274]. Elements in the Table are satisfactory after JD2433150. The shape of the light curve apparently varies. QS Aql Min II 5.97. VB (A 6.5m; B 6.7m, 0.18", 137deg). P var. QV Aql The epoch of main Max is given. QY Aql d = 0.016P. P var? V0336 Aql B - V: +1.17, +1.55. V0337 Aql Min II 9.09. P var. 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 increases (see also [02265, 04493]). Before JD2435600 Min = 2428023.550 + 3.390842d*E. Halpha emission observed at Max light [08074]. The shape of the light curve and d apparently vary. Delta(m) probably decreases [08075]. V0343 Aql Min II 10.7. V0346 Aql Min II 9.1. ADS 13438 A (B 11.3m, 2", 245deg). Elements in the Table are valid after JD2437000. The shape of Min I varies [07001]. V0348 Aql d ~0.08P. V0352 Aql The nucleus of the supposed planetary nebula P.K. 37-3.3deg. V0356 Aql VB A (B 0.2"). V0367 Aql The elements are satisfactory 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: +1.51d*10**(-9)*E**2. V0409 Aql Min II 12.2. Spectral type from another publication is A2 - A3. V0411 Aql Epoch of Min is given. V0417 Aql Min II 11.5. P var. Before JD2439000: Min = 2428427.127 + 0.3701251d*E. V0421 Aql P var? V0423 Aql Elements are valid for JD2426900 - 28000. During JD2429020 - 31670 the waves are much longer or absent. V0433 Aql Waves of 26d - 80d duration with Delta(m) = 0.1m - 0.9m. The mean light varies according to the formula Max = 2438312 + 648d*E. V0449 Aql The star in [01091, 02282] is actually not identical to HV5424. V0461 Aql Close component ~15.5m, the range of combined light is given. V0467 Aql Waves of 40d - 72d duration. The mean light varies with P ~1400d. V0473 Aql P ~330d is sometimes observed. V0476 Aql EW type with doubled period is possible. Elements are based 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 JD2428000. V0497 Aql VB A (B 16.5m, 9", ~0deg). V0524 Aql The variable is np from the star shown in the chart in [02317]. V0527 Aql IS type is possible. V0528 Aql VB A (B 16.5m, 11", 59deg). V0535 Aql VB [01943], two components are seen on Palomar prints, eastern of them being red. According to [01943], rapid 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. See also [08637]. JD2433631.8421 + 0.716292d*E. See also [02124]. V0586 Aql Irregularities are sometimes observed, but then the periodicity is probably resumed. V0596 Aql Resembles S Vul. V0599 Aql Min II 6.73. According to [08083], may be constant. V0600 Aql B - V: +1.36, +1.70. Before JD2428000 another value of P is possible [08632]. V0602 Aql d = 0.02P. Min II 12.7. V0603 Aql SB (P = 0.13854d [03169]). Outside the outburst there are variations of light (eclipses) with Delta(m) = 0.30m, Min I = 2444401.399 + 0.1377d*E (D ~0.2P). The shape of the light curve and the depth of minima differ from cycle to cycle. The brightness in minima shows fluctuations apparently connected with the presence of a hot spot [04500]. V0605 Aql A unigue variable. 8" np from a 17m star. Min ~20m pg. Photographs of the field [06041, 06042]. The light curve resembles those of the SN in NGC 1058 or of eta Car [06040]. The only Max observed, with fluctuations, occured in 1918 - 1924. In 1921 the spectral type was found to be R [02464]. The star is inside the old 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) [01091]. 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 [01091]. V0663 Aql P = 194.5d is possible. V0666 Aql The range is given for combined magnitude with a preceding 16.5m star. Separately was found ~17m pg near Min. V0672 Aql P var? Blazhko effect is possible [03113]. 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 the variable [01881] 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 brightness with P ~1350d (JD2437124 - 40512) [06025]. According to [00773] waves with P ~100d - 150d (JD2427543 - 31318). V0714 Aql d = 0.05P. V0724 Aql Min II 11.57. V0733 Aql P var? Before JD2434500, possibly Max = 2434453.72 + 6.17687d*E [00001]. 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 [03165] 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 slow ones. May belong to "polars" of XPRM type. Peculiar spectrum with broad emissions and blue continuum [08676]. V0800 Aql VB. According to [06072] 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 of the light curve varies.(U - B) index in Min I is redder and Min II is bluer than average. V0829 Aql Twice longer P is possible. V0836 Aql RR type is possible ([00085]; it is suggested also by the spectrum [08676]). V0850 Aql In the centre of the planetary nebula P.K. 37-6.2. V0866 Aql Min II 14.8. According to [06026], the depth of Min II 0.4m, EB type. V0867 Aql P var? V0871 Aql Min II 14.5, Min II - Min I = 0.425P. Physical changes in the range 13.3 - 13.6 are possible. Eclipses start from the 13.6m level. 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 [06004], 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 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. Apsidal motion is possible. V0890 Aql Nova Aql 1946 = asteroid N258 Tyche [09038]. V0891 Aql Min II 15.8. V0895 Aql P var. Max = 2430931.435 + 0.265108d*E (JD2426920 - 35010) [02267]. 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 is given in [08717] 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 [01884]. Similar to EW Lac. He lines are widened by the rotation, NaI lines are narrow. Light changes are periodic: Min = 2436458.66 + 0.8518d*E. The cause of variations is probably connected with the rotation and the inhomogeneous brightness distribution over the disk of the star [03178]. Profiles of spectral lines vary. The expansion of the envelope terminated in 1965, which apparently led to the development of inhomogeneities and to the broadening of hydrogen line profiles [04525]. V0925 Aql Some observers found constant brightness [03165]. V0929 Aql Short period. V0936 Aql Short period. V0947 Aql According to [05412], rapid irregular changes are not excluded. According to [00504], 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 (JD2421871 - 28105). V0958 Aql VB A (B 17.0m, 0.2' np; C slightly brighter, 0.1'f). 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 [04260], P = 110d. V0998 Aql The position coincides with the planetary nebula P.K.50-3.1deg. V0999 Aql Tsessevich's observations [07806] do not agree with the elements in the Table. V1017 Aql Elements need confirmation. V1033 Aql P var? V1045 Aql Min II 13.5. V1046 Aql P var? [08321].Min = 2427713.314 + 5.28303d*E [04027]. 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 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 [03156]. 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 [04564], constant. In [03932] was not separated from a close component which probably led to distortions 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 field variations. The epoch of minimum intensity of the magnetic field is given. V1295 Aql Shell star. Dramatic spectral changes were observed [05240]. The variability is hardly periodic, though P ~100d is possible. Sometimes light fluctuations on several days' time scale are observed [05880]. IR excess [06277]. For a detailed spectroscoric study, with evidence for the outflow of matter from the surface, see [04739]. Considerable magnetic field [04435]. V1297 Aql d = 0.05P? Min II 14.5. V1298 Aql mu alpha = -0.0392s, mu delta = -1".330. The companion of the star BD +4deg 4048 (ro = 73".8, theta = 151.5 deg). 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. OH, H2O, SiO maser. According to [07437], the energy distribution in the IR spectrum (1 - 22mkm) resembles that of eta Car. Emissions of neutral metals are observed in the spectrum. Increased in brightness during 1925 - 1970; Max ~1970. V1323 Aql Close VB; var - northern component. V1325 Aql VB, np component var. V1331 Aql Min II 7.95. According to [04619] P = 1.364076d. V1333 Aql Aql X-1. Light variations with P ~1.28d - 1.31d due to orbital motion are possible [04625]. Bursts characteristic of the XB type are observed [04757]. Lx/Lopt ~500 outside 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 light varies in the range 14.0 - 14.6 V according to the elements Max = 2443662.5 + 165.5d*E [00512]. The depth of Min I varies from 0.2m to 0.9m V, the depth of Min II varies from 0 to 0.4m V. Two systems of H, HeI, HeII emission lines are observed in the spectrum: the "stationary" system corresponding to Vr changes from 300 to 150 km/s with P = 13.1d, and the "relativistic" one, corresponding to Vr changes from +50000 to -35000 km/s with P = 165.5d. The spectral study [00535]. The system apparently consists of an O - B star filling its inner Roche lobe and a compact object surrounded by an accretion disc wich is precessing with P = 165.5d. Two jets consisting of dense condensations of matter emerge from the system with relativistic velocity (0.27 c) in opposite directions. The luminosity of the disc amounts to not less than 60% of the total luminosity of the system [00926, 00953]. The object may be a former supernova which bursted not 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), P = 7.176455D (JD2395100 - 2412100). Since JD2412100 - see Table. For the whole interval Max = 2442794.773 + 7.176735d*E + 2.18d*10**(-8)*E**2 [08632]. In the UV band the light of a possible A0V comparion is apparent. sig Aql ADS 12737 A (B 12.34m, 48", 328deg). Depth of Min II 0.1m. In [04627] P = 1.950271d is given according to spectroscopic data. R Ara Min II 6.2. VB A (B 8.2mV, 4", 123deg). S Ara (k - b)2 = 0.09. P var [01932, 03126]. Max = 2416284.792 + 0.45188910d*E (JD2414000 - 19000);Max = 2419149.797 + 0.45188581d*E (JD2419000 - 30000) [00752]. Since JD2441000 - see Table. For the whole interval, with sufficient accuracy, Max = 2420047.2382 + 0.451888176d*E - 1.36d*10**(-10)*E**2 [03126]. T Ara VB A (B 11.0m, 34", 60deg). X Ara Shown in the chart for S5809. RT Ara According to Cannon [01944] who discovered the star's variability, a companion 12.0m is present in 0.1m to W and somewhat to the north from the variable. Cannon points out that at Min light the variable becomes fainter than the companion. No sign of the companion's existence was found by Hoffmeister [00016] and by Payne-Gaposchkin [00624]. According to [00624], the mean cycle is ~78d, and RVA type is possible. RW Ara d = 0.022P. Min II 8.91. Changes of the shape of the light curve due to gaseous streams or a hot spot are possible. TT Ara ZrO bands may be present in the spectrum [03181]. TV Ara In the region of the cluster NGC 6208. TX Ara VB A (B 16.5m). Twice shorter period is possible. XX Ara Min II 14.1. YY Ara The star's being an eclipsing or irregular variable is not excluded [00424]. AA Ara Min II 13.3. AD Ara [A/H] = -0.4. AE Ara VB A (B 12m, 0.3' sf). P.K. 344-8.1. A compast planetary nebula or a symbiotic star. Irregular abrupt brightenings by 3m - 4m separated by several years are observed [00255]. The spectral data are discussed in [08076]. 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; since JD2425000 - see Table. DU Ara B - V: +0.52, +0.84. P var. Max = 2418145.560 + 1.63999d*E (JD2411000 - 21000); Since JD2425000 - see Table. EK Ara VB A (B 15m). EL Ara Before JD2420400 Max = 2415140 + 332d*E; since JD2425000 - see Table. ER Ara Min II 14.2. EV Ara Before JD2420400 Max = 2413750 + 237d*E; since JD2425000 - see Table. EZ Ara P var. FU Ara The depth of Min I is 0.97m and 0.89m, the depth of Min II is 0.20m and 0.23m in blue and yellow light, respectively. GK Ara Before JD2417800 Max = 2414050 + 237d*E, since JD2418400 - see Table. GM Ara Min II 12.8. HX Ara B - V: +0.23, +0.36. A hump on the ascending branch (phi = 0.93P) [08118]. KY Ara Only one sharp Max (JD2428715 - 712) was observed. Possibly a Nova. KZ Ara VB A (B 14.1m sp). LP Ara d = 0.04P? Min II 10.5? LQ Ara In 1959 rapid variations at times for 0.5m near 11m were observed; surrounded by a nebula [04001]. 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 accompanied by colour changes. Possibly an eclipsing variable [04678]. 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: -4.4d*10**(-11)*E**2. V0536 Ara Min II is present. EB type is possible. P var. P = 2.374101d (JD2415000 - 22000); since JD2422000 - see Table. V0539 Ara VB A (B 9.22m, 12", 269deg). Min II 6.09, d = 0.01P. 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 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 [01356]. Modulation with P ~4h and the amplitude up to 40% was found in the broad band optical flux [04944]. 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 eclipsing binary or (more probably) an object similar to rotating variables of ACV type. V0821 Ara 4U 1658-48. Unusua1 X-ray system. Quasiperiodic optical variations (P ~20s) with total amplitude 40 percent, abrupt bursts on ~20 ms time scale leading to two-fold flux increase and light changes by 6m during less than two months were observed [04958]. Lx/Lopt = 3. V0870 Ara Type DSCT: is also possible. R Ari OH emission. T Ari P var. Max = 2417160 + 313.5d*E (JD2404800 - 17200); Max = 2434616 + 323.1d*E (JD2419400 - 34560). Since JD2436560 - see Table.
= 319.53d
(JD2404800 - 44160). Sometimes A < 1.5m.
U Ari SiO maser.
V Ari Vr = - 180 km/s.
W Ari Maps given in [02544, 06067] are wrong.
X Ari B - V: +0.28, +0.56. P var. Max = 2420785.635 +
0.6511248d*E (JD2420460 - 33210) [03506]. Since
JD2433210 - see Table. [Fe/H] = -2.17.
RR Ari Min II 6.75:; Min II - Min I = 0.55P. Variability is not
confirmed by other authors' photoelectric observations.
V = 5.75.
RS Ari Min II 11.0.
RU Ari OH emission.
RV Ari B - V: +0.29, +0.44. 0.34P =< M - m =< 0.53P.
P1 = 0.07195d [08137]; P2 = 0.27554d [07033]. Moments of
brightest light maxima T = 2435066.400 + 0.31632996d*n
[02290].
RW Ari B - V: +0.35, +0.46. P var. Max = 2428183.324 +
0.3543184d*E (JD2428040 - 36700) [03188]. Since
JD2440900 - see Table. According to [06043] - EA type:
Min I = 2439384.97 + 3.1754d*E. Total light range
(11.47 - 13.25 V) [08127] seems doubtful. It is not
excluded that the eclipses and light increase of RW Ari
given in [08127] are explained by variability of one of
comparison stars used.
RX Ari d = 0.02P. Depth of Min II 0.10m.
SS Ari P var. Min II 10.82:.
ST Ari P var. Max = 2427347 + 94.2d*E (1933 - 1939); Max =
2429525 + 106.6d*E (1939 - 1942); Max = 2430588 +
95.2d*E (1942 - 1946); Max = 2432118 + 100.0d*E
(1946 - 1961). Mean elements are given in the Table.
SX Ari B - V: -0.10, -0.12. Epoch of Min is given.
SZ Ari d = 0.03P.
TT Ari Porb = 0.137551d [08138]. Along with light variations
typical for Z Cam variables there are sinusoidal variations
with amplitude of about 0.2m B and variable period:
P = 0.1329d (1961 - 62), P = 0.1327d (1966) [04931],
P = 0.1326d (1978) [04935]. Sinusoidal variations are
superimposed by quasiperiodic oscillations up to 0.2m with
8 - 20 minutes cycle and irregular flickering up to 0.1m
in 1 minute.
TU Ari P var. Max = 2420463.353 + 0.4716219d*E
(JD2420463 - 34720). Since JD2436820 - see Table.
TV Ari P var.
TX Ari P var?
TY Ari Form of the light curve varies. Mean value of the period
is given.
UV Ari The second overtone period given in the
Table is dominating. Sometimes the fundamental
period P0 = 0.062d and the first overtone period P1 =
0.047d are observed.
UW Ari Amplitude varies. In the interval JD2441581 - 693 - const.
[07544].
UX Ari T = 2440133.766 + 6.43791d*E [06444], where T is epoch of
conjunction (G5 component is behind K0 component).
Brightness varies in waves with a period ~Porb, but the
phase psi of light minimum calculated according to the
elements given above changes with time: psi = 0.1P
(1972 - 1974), psi = 0.8P (1976), psi = 0.7P (1977),
psi = 0.6P (1978). Mean brightness varies, amplitude of
the wave varies from 0.04m up to 0.15m.
VW Ari BDS 1269 A (B 8.33m, 74", 31deg). P2 = 0.089d.
Metal deficiency. The companion has normal metal abundance.
VY Ari SB? Epoch of Min is given.
Second light variation is also observed: Min =
2442044.6 + 43.9d*E. A small flare in U band was
observed.
gam Ari VB A (B 4.65m, B 9 V, 7.9", 0deg). Epoch of Min is given.
R Aur VB A (B 8.6m, 48", 239deg). P var [07165];
cycle 64.5a is possible.
S Aur P var. In the early fourties of our century the star was
faint with small and irregular variations.
T Aur Min = 2437614.0088 + 0.20437851d*E [08145]. P var?
var: Max = 2424334.6612 + 0.44775262d*E
(JD2417400 - 33610) [00323]. Since JD2433850 - see Table.
Light curve and period vary with the Blazhko effect
period Pi = 225.5d [06464]. Semiamplitude of deviations
from linear elements is +-0.032d. 0.14P <= M - m <= 0.25P.
(k - b)2 = 0.05.
RW Cap d = 0.020P. Min II 9.9. P var. Min I = 2418924.594 +
3.3923922d*E (JD2418920 - 24000) [06774];
Min I = 2424003.014 + 3.3923457d*E (JD2424000 -
34500) [02389]; 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 [01331].
TW Cap P var. P = 28.6421871d (JD2414000 - 17600);
P = 28.61700115d (JD2417600 - 24000) [01331];
Max = 2426211.90 + 28.59497d*E (JD2421400 -
26200) [02390]; Max = 2435664.8 + 28.5578d*E
(JD2426210 - 37500) [02309]; since JD2437500 - see Table.
0.14P <= M - m <= 0.40P. [Fe/H] = -0.72.
TY Cap Min II 10.6. P var. Min I hel = 2432017.956 + 1.423466D*E
(JD2425500 - 35000); since JD2435000 - see Table.
UW Cap Min II 11.5; Min II - Min I = 0.5P. P var? Min I =
2434627.290 + 1.399118d*E (JD2427000 - 35000);
since JD243500 - see Table.
YZ Cap (k - b)2 = 0.08.
AD Cap Outside eclipses B - V = +1.00. P var?
AE Cap Mean brightness varies with P = 2300d.
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,
1911); mu = 0.391", P = 138.8deg. Min II 2.90.
The light curve shape var? [03305].
eps Cap VB A (B 9.52m, 68.7", 47deg).
R Car VB A (B 12m, 2.1", 138deg). H2O, SiO maser.
U Car P var. Max = 2429023.80 + 38.753d*E (JD2415000 -
29500); since JD2429500 - see Table.
V Car The light curve shape var?
X Car Min II 8.6.
Y Car VB A (B 12.22m, 15"; C 12.96m, 30"). SB (P = 400 - 600d)
[05119]. The fundamental mode period P0 is given in the
Table (A = 0.58m). The first overtone period P1 = 2.55954d
[05119] (A = 0.28m). P1/P0 = 0.7032.
RR Car P var. = 154d (JD2421500 - 23500); = 259d
(JD2426400 - 30100); = 154d (JD2430400 - 33100).
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.
Max = 2418475 + 416d*E (JD2415140 - 18500);
Max = 2429901 + 417.3d*E (JD2423600 - 32900);
since JD2434100 - see Table.
ST Car Depth of Min II 0.27m.
SW Car Depth of Min II 0.05m.
SZ Car In the region of the cluster NGC 3114.
TX Car The light curve shape var?
TZ Car Mean brightness varies with P = 1183d; the amplitude of
the short cycle is large in mean brightness maximum and
small during its minimum.
UX Car In the region of the cluster IC 2581.
VV Car In the region of the very poor cluster N 99 [07374]
(10h 36.0m -58deg 56', 1950.0) embedded in a nebula.
VY Car VB A (B 11.07m; B 9V:, 10", 150deg). P var.
Nonlinear term: -0.000021d*E**2 (JD2410000 - 44200).
The latest observations may be represented also by linear
elements: Max = 2444161.16 + 18.9138d*E
(JD2441000 - 44200). [A/H] = 0.4.
WZ Car P var. Max = 2419981.099 + 23.000945d*E (JD2410000 - 20000)
[00025]; Max = 2423984.12 + 23.0054d*E (JD2419800 - 25500)
[00322]; Max = 2434914.86 + 23.0075d*E + 0.000025d*E**2
(JD2434500 - 41200) [02309]; since JD2434500 - see also
Table.
XX Car P var. Max = 2420769.703 + 15.723704d*E (JD2410000 - 22500)
[00025]; P = 15.7196d (JD2423000 - 30000) [00003]; since
JD2434500 - see Table; elements given in the Table contain
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
JD2435000 - see Table.
AG Car Central star of the low-excitation planetary nebula
P.K.289-0.1 ejected probably during a nova-like outburst
of the star about 1000 years ago [07052, 07113].
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
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
(Min brightness).
DI Car Besides Cepheid-like light variations with the amplitude
1.7m and elements Max = 2438553.70 + 29.210d*E
(JD2438465 - 40300) [05324] large weakenings of brightness
are observed [04678]. 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)
[00046, 02309]. Since JD2435300 - see Table.
FK Car VB.
FO Car VB A (B 14m, 7", 90deg). P var. Max = 2434922.531 +
10.3559d*E (JD2423700 - 35300) [06006]; since JD2436000
- 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 [07374] (10h
36.0m -58deg 56', 1950.0) embedded in a nebula. Min II
10.9.
FT Car According to [02197] spectrum C. Misidentification is
possible.
FV Car VB A (B 13m, 10", 135deg). P var. There are two additional
terms in the elements given in the Table:
-0.1065d*10**(-7)*E**2 - 0.584d*10**(-11)*E**3.
d = 0.02P:. Min II 13.0.
GG Car Min II 9.5. Gas and dust envelope.
GH Car 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.
System with the apsidal motion; e = 0.157, omega = 99deg.
There are sinusoidal terms in the elements for Min I given
in the Table: +0.121d sin(0.094389deg*E) -
0.007d sin(0.188778deg*E);
Min II = 2424263.236 + 2.4222338d*E -
0.121d sin(0.094389deg*E) - 0.007d sin(0.188778deg*E).
DII = 0.17P.
GM Car In the region of the very poor cluster N 99 [07374] (10h
36.0m -58deg 56', 1950.0) embedded in a nebula.
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
an amplitude 0.16m are given in the Table. For the first
overtone oscillation with an amplitude 0.07m
Max = 2440742.4 + 2.93424d*E. Epochs of maxima and
amplitudes are given according to [05175].
HH Car VB A (B 13.0m, 5", 260deg; C 11.11m, 13", 337deg; D 12.65m,
15", 7deg). d = 0.02P. Min II 10.66. P var [08094].
Min I hel = 2430860.162 + 3.2315393d*E (JD2427590 - 35260)
[05292]. Possible current elements are given in the Table.
HI Car Min II 10.8.
HK Car VB A (B 12.5m, 4"). Range of combined brightness variation
is given.
HL Car d = 0.03P:.
HN Car Min II 12.5.
HP Car VB A (B 9.1m, 0.4", 178deg). Min II 9.3. Elements should
be corrected [08083].
HQ Car B - V: +0.63, +1.04.
HR Car Spectrum description [01914, 06466].
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
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 [00085] is wrong by 3deg. Identical to
V336 Car, see [06316].
KQ Car Min II 10.3.
KU Car Min II 11.6.
MP Car VB A (B 16m, 180deg).
MZ Car sf component of a close pair.
OO Car Min II 14.7.
OV Car Min II 13.5.
OY Car Eclipse elements:
Min I hel = 2443993.553241 + 0.0631209247d*E [05185];
D = 0.050P, d = 0.044P. The hump on the light curve is
observed at the phase of 0.75P. Depth of Min I varies
between 1.48m and 2.47m.
PT Car Min II 13.0:.
PX Car Min II 10.10.
QR Car Min II 10.4.
QS Car Min II 9.3.
QU Car HDE 310376 (HA 112, 173). Flickering resembles V818 Sco.
Variations by 0.2m in 90s were observed. No periodicity
was found. Emission lines He II 4686, CIV - NIII 4630 -
4650 and sometimes weak hydrogen absoptions (corresponding
to A or B type) are noticeable in the spectrum [05643].
QX Car Min II 7.02.
QY Car In the open cluster No.90 [07374].
QZ Car In the eta Carina nebula, possible member of the cluster
Collinder 228. Min II 6.43. Two SB1 systems (A and B),
B is eclipsing (A: SB1, P = 20.73d, O9.5 I,
Delta(m) = 0.6m). Combined brightness is given.
V0341 Car In the variable reflecting nebula IC 2220. In the region
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 [04627]).
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
cluster Tr 16. A very massive young star surrounded by an
expanding gas and dust shell with the diameter 2" at 2mu
and 6.5" at 12.2mu. Maximum brightness was observed in
1843. Since 1880 varies in the range 5.9 - 7.9 V. In the
interval JD2434000 - 41000 Max = 2434037 + 1110d*E. There
are emission lines of H, HeI, FeII, [FeII], etc. in the
spectrum. Description of the spectrum [05251, 07279].
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;
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);
Max = 2432870 + 413.6d*E (JD2427060 - 32870);
Max = 2437948 + 423.0d*E (JD2432870 - 39210).
Current elements are given in the Table.
Y Cas OH, H2O emission; SiO maser.
Z Cas SiO maser.
RS Cas P var. Max = 2416942.16 + 6.29552d*E (JD2412650 - 34900)
[03317]. Since JD2434900 - see Table.
RV Cas There are signs of Se type in the spectrum [03383].
RW Cas P var. Max = 2421354.22 + 14.8004d*E (JD2417000 - 30000).
Since JD2430000 - see Table. [A/H] = 0.3.
RX Cas Unigue rapidly evolving eclipsing system. 9.12<=Min II<=9.49;
Min II - Min I = 0.5070P. P var. Nonlinear term:
+1.017d*10**(-5)*E**2. Observations may be represented
also by three systems of elements: Min I =
2416250.889 + 32.31481d*E (0 <= E <= 286,
JD2416250 - 25482); Min I = 2416248.835 + 32.32145d*E
(331 <= E <= 554, JD2426940 - 34155);
Min I = 2416244.990 + 32.32765d*E (734 <= E <= 876,
JD2439970 - 44570). Brightness of the system out of
eclipses periodically varies within 8.6m - 9.0m with
elements Max = 2416198 + 516.06d*E [05036]. Max - Min =
233d = 0.45P [00881]. Strong emissions of H, NV, CIV,
SIIV, FeIII. Powerful gaseous stream and accretion
phenomena are possible.
RY Cas [A/H] = 0.0.
RZ Cas Min II 6.26. The light curve shape var; d var
(0.000P <= d <= 0.009P). P var, variations are irregular.
Mean elements based on visual and photographic
observations: Min I = 2416886.8806 + 1.195253065d*E
(JD2416800 - 26700) [08820], Min I = 2432820.7853 +
1.1952517d*E (JD2426700 - 34000) [00938]. From
photoelectric observations: Min I = 2432115.5827 +
1.1952472d*E (JD2429870 - 30400); Min I =
2432085.7011 + 1.195259d*E (JD2432000 - 32460);
Min I = 2434349.5130 + 1.1952525d*E (JD2432450 - 34420);
Min I = 2434703.3035 + 1.195238d*E (JD2434420 - 34705);
Min I = 2435934.4087 + 1.1952499d*E (JD2434705 - 35950);
Min I = 2438829.2818 + 1.195243d*E (JD2436800 - 39100);
Min I = 2440182.3089 + 1.195259d*E (JD2439380 - 40200);
Min I = 2441333.3257 + 1.195244d*E (JD2440500 - 41350);
Min I = 2442327.7798 + 1.1952521d*E (JD2441550 - 42350);
since JD2442850 - see Table.
SU Cas [A/H] = -0.1.
SV Cas P var. Max = 2421839 + 279.3d*E (JD2417600 -
21900); Max = 2430450 + 281.7d*E (JD2422500 -
31900); since JD2432600 - see Table.
SX Cas VB A (B 11.5m, 19", 250deg, 1966). Min II 9.32. The light
curve shape var. DII = 0.171P:, dI = 0.036P, dII = 0.050P.
P var. Min I = 2433963.267 + 36.56727d*E (JD2418000 -
37000); since JD2438700 - see Table. Strong emissions
of H, NV, CIV, SIIV, FeIII. Gaseous streams and accretion
phenomena.
SY Cas VB? P var. Max = 2417911.547 + 4.070969d*E
(JD2417000 - 34000); since JD2434000 - see Table.
SZ Cas P var. Max = 2421261.66 + 13.6009d*E (JD2416700 - 21260);
Max = 2426650.20 + 13.6072d*E (JD2421260 - 27170) [08821];
Max = 2429727.240 + 13.61744d*E (JD2427170 - 33050);
Max = 2436810.92 + 13.62655d*E (JD2433050 - 38720);
since JD2438720 - see Table. [A/H] = -0.6.
TU Cas Fundamental mode period P0 is given in the Table; the
corresponding amplitude is 0.69m. First-overtone period
P1 = 1.51830d; the corresponding mean amplitude decreased
from 0.4m to 0.25m during 67 years [05078]. P1/P0 = 0.71.
M - m var (0.17P <= M - m <= 0.35P).
TV Cas d = 0.01P. Min II 7.34. The light curve shape var.
Period of these variations - 600d [08822]. P var. Mean
elements based on visual and photographic observations:
Min I = 2432827.7665 + 1.81260983d*E (JD2415650 - 32800)
[01926]. From photoelectric observations Min I =
2432827.7665 + 1.8126142d*E (JD2432800 - 36490);
Min I = 2436483.8091 + 1.81255d*E (JD2436480 - 36980);
Min I = 2438472.2386 + 1.81263d*E (JD2437000 - 38500);
Min I = 2438829.3230 + 1.8126048d*E (JD2438470 - 41750);
since JD2441750 - see Table.
TW Cas Min II 8.40.
TX Cas Min II 9.6.
TY Cas P var. Max = 2419260 + 545.0d*E (JD2419200 - 25300);
Max = 2428965 + 623.8d*E (JD2427000 - 41500);
since JD2441500 - see Table.
UU Cas Min II 10.5.
UZ Cas [A/H] = -0.3.
VV Cas P var. Max = 2422514.16 + 6.207510d*E (JD2417000 - 32500);
since JD2432500 - see Table. [A/H] = -0.2.
VW Cas [A/H] = 0.0.
WY Cas In the region of the cluster NGC 7789.
The spectrum of the G type star is seen in minimum light
[03502]. The existence of a physical companion is possible.
S6/6-e.
WZ Cas VB A (optical companion B 8.7m, 58", 89deg). SC7/10e.
Light variations are sometimes taking place with doubled
period.
XX Cas Min II 10.2.
YZ Cas VB A (B 11.23m, 35", 160deg). d = 0.045P. Min II 5.78.
ZZ Cas Min II 10.9.
AB Cas EA/SD. Min II 10.28. P var. Min I = 2430755.678 +
1.366863d*E (JD2425400 - 33150); Min I =
2433616.532 + 1.366876d*E (JD2433150 - 37000);
Min I = 2440475.5216 + 1.3668783d*E (JD2437000 -
41600); since JD2441600 - see Table.
The A3 component is a DSCT type variable with the elements:
Max hel = 2444912.1759 + 0.0582874d*E [08825]; amplitude
of pulsations Delta(V) var (0.03m <= Delta(V) <= 0.09m).
AE Cas Min II 12.8.
AH Cas Min II 13.3.
AL Cas Min II 13.6.
AO Cas Min II 6.24. The light 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;
D 9.8m, 76", 268deg; E 11.28m, 43", 115deg; F 11.06m, 69",
338deg; G 11.11m, 67", 348deg). Min II 4.86;
Min II - Min I = 0.614P; DII = 0.076P; dII = 0.037P.
AS Cas VB A (B 15.5m, 3", 45deg).
Fundamental mode period P0 is given in the Table; the
corresponding amplitude is 0.59m. First-overtone period
P1 = 2.2909d; amplitude of oscillations with this period
is 0.13m. P1/P0 = 0.76.
AX Cas Min II 12.9.
AZ Cas B - V: +1.78, +2.20. D = 110d, d = 88d = 0.026P.
BD Cas B - V: +1.50, +1.61. P var. Max = 2429124.84 +
3.65129d*E (JD2415000 - 29130) [00915];
since JD2429130 - see Table.
BE Cas VB A (B G, 25", 260deg).
BH Cas According to [00453] there are no variable stars on the
place of BH Cas and in its surroundings.
BM Cas Min II 8.98. Shape of the light curve varies. P var.
There is a periodic term in the elements:
+2.6d*sin(7.11deg*E + 104deg).According to [00939], on the
light curve cepheid-like variations are observed with
P = 27d.
BN Cas Min II 13.4.
BS Cas Min II 12.6.
BU Cas D = 0.02P.
BY Cas In the region of the cluster NGC 663. P var.
Max = 2416871.91 + 3.2218d*E (JD2416800 - 24860) [00921];
Max = 2431929.60 + 3.221297d*E (JD2426900 - 34300);
Max = 2438399.629 + 3.222588d*E (JD2436200 - 39400);
since JD2439400 - see Table.
BZ Cas Min II 11.5.
CC Cas Min II 7.26. The light curve shape var? P var?
CE CasA Possible member of the cluster NGC 7790. VB A (B = CEb Cas,
2.4", 265deg).
CE CasB VB B (A = CEa Cas). 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
with cycles from 110d to 250d.
CR Cas Min II 13.3.
CS Cas [A/H] = -0.4.
CV Cas Epochs given in [00922] are not represented by the elements
given in the Table. P var?
CW Cas Min II 11.47. Shape of the light curve and depths of
minima vary. P var. Min I = 2435745.6163 + 0.31886497d*E
(JD2432400 - 41000) [03332]; since JD2441000 - see Table.
CY Cas [A/H] = -0.7.
DD Cas P var. Max = 2415612.45 + 9.807272d*E (JD2415600 - 18600);
since JD2418600 - see Table. The star may be a member of a
binary system with Porb = 8500d +- 1000d.
DF Cas In the region of the cluster NGC 1027.
DI Cas P var. Max = 2432068 + 371.7d*E (JD2417200 - 32100);
since JD2432100 - see Table.
DL Cas Member of the cluster NGC 129. [A/H] = 0.0.
DN Cas Min II 10.13.
DO Cas Min II 8.61; dI = 0.08P.
DP Cas Min II 13.6.
DZ Cas Min II 12.0.
EG Cas Min II 13.1.
EK Cas Depth of Min II 0.05m.
EM Cas P var. Max = 2433132 + 283d*E (JD2427700 - 33150); since
JD2433150 - see Table. Amplitude strongly varies.
EN Cas Min II 12.4. P var.
EP Cas Min II 11.4.
EQ Cas Min II 12.7. P var. Min I = 2432150.04 + 58.26d*E
(JD2432200 - 34060) [03336]; 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 +
3.758738d*E (JD2424800 - 39500) [00936];
since JD2439500 - see Table.
GK Cas Depth of Min II 0.05m.
GT Cas d = 0.02P.
GU Cas Min II 11.3. P var. Min I = 2428749.423 + 3.093329d*E
(JD2417470 - 35480) [00941];
Min I = 2437367.375 + 3.09325d*E (JD2435480 - 38750) [00001];
since JD2438750 - see Table.
GZ Cas Mean magnitude varies with P = 800d.
Max = 2428000 + 800d*E [00911].
HH Cas Epoch of Min is given. RV type is possible [00911].
HN Cas d = 0.038P.
HS Cas VB A (B 12m, 27", 15deg).
HT Cas Min hel = 2443727.93722 + 0.073647217d*E;
D = 0.13P. Depth of eclipses between outbursts is ~2.4 V.
Small quasi-periodic light oscillations with P = 100s.
Spectrum description [06163].
HU Cas P var. Max = 2417525.075 + 0.41159875d*E (JD2411600 -
28000); since JD2428000 - see Table.
IL Cas Depth of Min II 0.05m.
IR Cas Min II 11.5. P var. Min I = 2428750.2914 +
0.68069178d*E (JD2417500 - 38400) [00098];
since JD2438400 - see Table.
IS Cas Min II 12.2. P var. Min I = 2428776.262 +
1.8415172d*E (JD2417400 - 29500) [00098];
since JD2428000 - see Table.
IT Cas Min II 11.8; Min II - Min I = 0.553P; DII = 0.042P.
Apsidal motion is possible.
IV Cas Min II 11.3. P var. Min I = 2428991.302 +
0.9985232d*E (JD2416700 - 29000) [00098];
Min I = 2431438.648 + 0.9985056d*E (JD2429000 -
37700) [02263]; since JD2440000 - see Table.
IW Cas S4 +/6e.
IX Cas P var. Max = 2428749.39 + 9.15035d*E (JD2414700 -
29500) [00098]; Max = 2428749.90 + 9.1363d*E
(JD2428700 - 34350) [00944]; Max = 2437195.642 +
9.14783d*E (JD2434350 - 39100) [05462];
since JD2442000 - see Table. [A/H] = -0.4.
KL Cas Min II 12.3.
KO Cas P var. Max = 2425590 + 305.6d*E (JD2416700 - 26000);
since JD2426000 - see Table.
KR Cas Min II 9.9.
LR Cas Min II 10.9.
LU Cas Min II 14.3?
LW Cas In the apex of a small (8") bright cometary nebula in the
region of IC 1848. Novalike outburst was observed in the
interval JD2433900 - 34800. Infrared and radioemission.
LX Cas In the region of the cluster Collinder 33. Min II 15.3;
Min II - Min I = 0.47P; dI = 0.10P.
LY Cas In the region of the cluster Collinder 33. Min II 15.2.
MM Cas d = 0.08P: Min II 12.4.
MN Cas Min II 10.57.
MO Cas In the nebula NGC 7635. 10.2 - 13.1 I.
MP Cas In the nebula NGC 7635. 10.4 - 13.5 I.
MR Cas Min II 15.5.
MS Cas Min II 13.2.
MT Cas d = 0.04P. Min II 14.02.
MU Cas Min II 10.8.
MV Cas Min II 14.0.
MY Cas Min II 15.2. P var. Elements given in the Table are valid
since JD2438500.
NN Cas Min II 14.0.
NT Cas Min II 14.4.
NU Cas Min II 13.4.
NV Cas d = 0.03P.
OP Cas P var. Max = 2429109.726 + 5.510019d*E (JD2427950 - 34670)
[00176]; since JD2437000 - see Table.
OR Cas Min II 11.8. P var. Min I = 2429249.424 + 1.2457026d*E
(JD2413800 - 34800) [00176]; since JD2432000 - see Table.
OX Cas In the region of the cluster NGC 381. d = 0.016P. Min II
10.30; Min II - Min I = 0.512P. Apsidal motion [04524].
PR Cas P = 171d?
PV Cas Min II 10.36; Min II - Min I = 0.480P.
Depth of Minima probably varies. P var. Min I =
2428796.8142 + 1.75047346d*E (JD2415700 - 40000) [05302];
since JD2440000 - see Table. Apsidal motion [06253]:
Min II = 2428797.6894 + 1.75047346d*E -
0.040d*sin(0.0075deg*(E - 3000)).
PX Cas Min II 15.0.
PY Cas Epoch of Min brighness is given. Similar to RV Tau by
light curve shape [03348].
PZ Cas VB A (B 12.8m, WN 8:, 15", 100deg). OH, H2O emission.
QQ Cas Min II 10.8. P var. Min I = 2434330.169 + 2.142030d*E
(JD2415700 - 30000) [02530]; since JD2430000 - see Table.
QX Cas In the region of the cluster NGC 7790. VB A (B 13.1m, 3").
Min II 10.50; Min II - Min I = 0.37P; DII = 0.047P;
dII = 0.018P.
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,
whereas the chart [02345] leads to the nf component. It is
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
(JD2414600 - 35400) [02305]; since JD2434650 - see Table.
V0373 Cas An unique close binary. Porb = 13.4192d [04627]. Epoch
of Min I is given close to the epoch of one of
conjunctions. Min II - Min I = 0.58P. Maxima are very
sharp. Max - Min II = 0.25P. It is not excluded that the
star is an eclipsing one with physical variability of
components, but eclipses, if they exist, cause only a very
small part of the observed light variations. Range of
light variations is given according to [02651]. As a rule
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
which component varies. According to [04005] the range
of combined brightness variations is 0.26m.
According to [07051], 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
physical pair (p = 294") the bright component of
which is the dM2 star Wolf 46 = BD+61deg 195 (9.4).
V0392 Cas Min II 14.0. P var. Min I = 2429640.390 +
4.54094d*E (JD2425300 - 29640); Min I =
2429640.390 + 4.54064d*E (JD2429640 - 36900) [04027];
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
(JD2432850 - 37300); since JD2437300 - see Table. Period
variation may be cyclic. Mean elements:
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
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.
Tenuous shell ejected in 1975 is now falling back to
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
(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 +
0.2336882d*E (JD2428545 - 33570) [07008];
Min I = 2439029.461 + 0.23368912d*E (JD2439000 - 41300)
[07387]; since JD2440480 - see Table.
V0524 Cas OH, H2O emission. P = 163d?, 191d? 259d?, 620d?
V0526 Cas Two oscillations are superimposed: P1 = 0.0526d (A1 =
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
(JD2438580 - 39150); Max = 2441186.333 +
0.395683D*E (JD2440070 - 41250);
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
(A = 0.12", P = 15.9a); mu = 1.75", P = 98deg.
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
on a time scale of several minutes.
V0598 Cas VB A (B 12m, 19", 0deg). P = 2.825d? [02560].
V0615 Cas Variable radio source on 10.5 GHz; gamma - and X-ray
source?
V0627 Cas H2O emission.
V0635 Cas 4U 0115 + 634. SB (P = 24.3162d).
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
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;
D 8.5m, 64.4", 280deg.)
bet Cas VB A (B 13.7m, 31.3", 243deg); SB (P = 27d).
[Fe/H] = 0.64.
gam Cas VB A (B 11.0m, 2.2", 248deg; C 13.0m, 52.2", 348deg).
In HII region S 185. X-ray source MX 0053 + 60.
v sin i = 310 km/s.
del Cas VB A (B 11.5m, 31.7", 66deg). Min II 2.75. Min II - Min I =
361d. The elements given in the Table are still not
confirmed by anyone.
iot Cas VB A (B 6.89m, 2.3", 239deg; C 8.40m, 7.2", 114deg).
Astrometric binary (a = 0.113", P = 52.4a). Max (V) - Max
(lambda 1550) = 0.4P; A (lambda 1550) = 0.40m. The range
of total brightness variation of components A and
B is given.
kap Cas P = 0.09028d, P(Vr) = 0.14035d [02588]; P = 7d [08876].
omi Cas VB A (B 11.7m, 33.6", 303deg). SB1 (P = 1033d);
V sin I = 220 km/s.
pi Cas SB, Porb = 1.9642d.
rho Cas Usually varies within the limits 4.4m - 5.2m V.
In November 1945 the peculiar decrease of brightness began
lasting for 165d and in September 1946 the star reached
the middle of the deepest minimum (JD2432070) lasting for
320d. Then the brightness began to increase symmetrically
and by July 1947 the star attained its normal brightness
[00957]. Photographic magnitudes varied in the limits
5.4m - 8.3m. Spectrum description [08878].
B Cas Tycho Brahe's supernova. Stellar object is not identified
optically up to now.
R Cen VB A (B 12m, 28", 218deg). Epoch
of Min I is given. Min I 0.00P, Max I 0.23P, Min II
0.47P, Max II 0.64P.