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  omi And  
Andromeda Sequence
23 01 55.30 +42 19 34.0  (345.48042 +42.32611) Search nearby
B1950.0 22 59 37.05 +42 03 25.0
Galactic coord. 102.208 -16.096
Other names

(Internal only)
1 And AAVSO 2257+41 BD+41 4664
HD 217675 HD 217676 HIP 113726
HR 8762 SAO 52609  
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Variability type
Spectral type B6IIIpe+A2p
Mag. range
3.58 - 3.78 V
Discoverer --
Outburst --
Period --
Rise/eclipse dur. --
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1 GCVS Team 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 [E.H.Olsen, AsAp 20, 167, 1972.], 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 [H.Schmidt, ZsAp 48, 249, 1959.], Min I = 2436174.430 + 1.5998398d*E. The periodogram analysis shows a stable peak at P ~0.84d [M.BossI, G.Guerrero, L.Mantegazza, AsAp Suppl 29, 327, 1977.]. A possible shell event was observed late in 1975.
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1 MASCARA Variable star catalogue (online data) 2018arXiv180602247B
2 O. Burggraaff, G.J.J. Talens, J. Spronck et al., 2018, Studying bright
variable stars with the Multi-site All-Sky CAmeRA (MASCARA)
3 Photoelectric monitoring of bright Be stars. II 1992PASP..104.1160P
4 E.H.Olsen, AsAp 20, 167, 1972. 1972A&A....20..167O
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Revision History
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2 Otero, Sebastian Alberto 2007-03-02 18:39 UTC --
1 Admin, VSX 2005-12-17 20:33 UTC Initial database population.