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Line-profile variable ɛ Per: spectroscopic binary and (?) mild Be star

Published online by Cambridge University Press:  26 May 2016

A.E. Tarasov ,
V.V. Kostunin ,
P. Harmanec ,
J. Horn ,
P. Koubský ,
C. Blake ,
G.A.H. Walker  and
S. Yang
A.E. Tarasov
Affiliation:
Crimean Astrophysical Observatory, Nauchnyj, Crimea, 334413 Ukraine
V.V. Kostunin
Affiliation:
Crimean Astrophysical Observatory, Nauchnyj, Crimea, 334413 Ukraine
P. Harmanec
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, 251 65 Ondřejov, Czech Republic
J. Horn
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, 251 65 Ondřejov, Czech Republic
P. Koubský
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, 251 65 Ondřejov, Czech Republic
C. Blake
Affiliation:
Department of Astronomy, University of Western Ontario, London, Ontario, N6A 5B9 Canada
G.A.H. Walker
Affiliation:
Department of Geophysics and Astronomy, University of British Columbia, 129-2219 Main Mall, Vancouver, B.C., V6T 1Z4 Canada
S. Yang
Affiliation:
Department of Geophysics and Astronomy, University of British Columbia, 129-2219 Main Mall, Vancouver, B.C., V6T 1Z4 Canada

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ɛ Per (45 Per, HR 1220, HD 24760, ADS 2888A) is a star which was used for years as a spectrophotometric and MKK classification standard. Nowadays it is known as an archetype of early-type line-profile variables (LPV). The variations are so pronounced that they were misinterpreted for a composite spectrum (B0.5+A2) and the star was even reported to be a double-lined spectroscopic binary (Petrie 1958). Since 1983, the characteristics of line-profile variability in the spectrum of ɛ Per have been intensively studied (Bolton 1983, Smith 1985, Gies & Kullavanijaya 1988). The recent investigations of RV variations of ɛ Per led to the conclusion that ɛ Per is a spectroscopic binary with a period of about 14.05 days and a rather eccentric orbit (Harmanec & Tarasov 1990). The issue of the binary nature (with a very eccentric orbit) is of utmost importance since it could be causally related to the extremely large observed line-profile variations (e.g., Polfliet & Smeyers 1990, Tassoul & Tassoul 1992).

Type
5. Be Stars: Spectroscopy and Photometry
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 325 - 326
Copyright
Copyright © Kluwer 1994 

References

Bolton, C.T.: 1983, Hvar Obs. Bull. 7, 141 Google Scholar
Gies, D.R., Kullavanijaya, A.: 1988, ApJ 326, 813 Google Scholar
Harmanec, P., Tarasov, A.E.: 1990, Bull. Astron. Inst. Czechosl. 41, 273 Google Scholar
Petrie, R.M.: 1958, MNRAS 118, 80 Google Scholar
Polfliet, R., Smeyers, P.: 1990, A& A 237, 110 Google Scholar
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Tassoul, J.-L., Tassoul, M.: 1992, ApJ 395, 259 CrossRefGoogle Scholar