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Omicron Andromedae Photometry, Polarimetry, and a Tentative Model of the Light Variability

Published online by Cambridge University Press:  23 September 2016

K. Oláh ,
H. Božić ,
P. Hadrava ,
J. Horn ,
P. Koubský ,
S. Kříž ,
N.H. Minikunov ,
M. Muminović ,
J.R. Percy  and
A.G. Skcherbakov
...Show all authors
K. Oláh
Affiliation:
Konkoly Observatory, Hungarian Academy of Sciences, Box 67, 1525 Budapest XII, Hungary
H. Božić
Affiliation:
Hvar Observatory, Faculty of Geodesy, University of Zagreb, 58450 Hvar, Yugoslavia
P. Hadrava
Affiliation:
Astronomical Institute, Czechoslovak Academy of Sciences, 251 65 Ondřejov, Czechoslovakia
J. Horn
Affiliation:
Astronomical Institute, Czechoslovak Academy of Sciences, 251 65 Ondřejov, Czechoslovakia
P. Koubský
Affiliation:
Astronomical Institute, Czechoslovak Academy of Sciences, 251 65 Ondřejov, Czechoslovakia
S. Kříž
Affiliation:
Astronomical Institute, Czechoslovak Academy of Sciences, 251 65 Ondřejov, Czechoslovakia
N.H. Minikunov
Affiliation:
Crimean Astrophysical Observatory, Nauchnyj, Crimea, 334413, U.S.S.R.
M. Muminović
Affiliation:
Universitetsko Astronomsko Društvo, M.Tita 44, 71000 Sarajevo, Yugoslavia
J.R. Percy
Affiliation:
Department of Astronomy, University of Toronto, Toronto, Ontario, M5S 1A1, Canada
A.G. Skcherbakov
Affiliation:
Crimean Astrophysical Observatory, Nauchnyj, Crimea, 334413, U.S.S.R.
M. Stupar
Affiliation:
Universitetsko Astronomsko Društvo, M.Tita 44, 71000 Sarajevo, Yugoslavia
A.E. Tarasov
Affiliation:
Crimean Astrophysical Observatory, Nauchnyj, Crimea, 334413, U.S.S.R.

Extract

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Basic information about the star o and (HR 8762, HD 217675-6) is a bright (V=3.55m, B-V=-0.11m U-B=-0.50m) B6 III-Ve star. Its emission-line and shell spectrum is known to come and go on a time scale of years. In fact, the presence of a strong shell spectrum misled the authors of the HD catalogue to assign the star two HD numbers.

o and is a prototype of Be rapid light variables in the sense that it has the longest record of photoelectric monitoring which goes back to 1915! The long history of attempts to understand the variations of this star has recently been summarized by Harmanec (1983). Collecting and analyzing all historical photoelectric observations, Harmanec (1984) concluded that the light variations of o And can be understood as a superposition of a long-term cyclic (8.5y) variation with an amplitude over 0.1m (the star being faintest at the recorded shell maxima) and a rapid periodic variation with a period of 1.571272 days.

Type
IV. Models
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 456 - 459
Copyright
Copyright © Cambridge University Press 1987

References

Reference list

Harmanec, P. (1983). Hvar Obs. Bull. 7, 55.Google Scholar
Harmanec, P. (1984). Inf. Bull. Var. Stars #2506.Google Scholar