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Be Stars as Interacting Binaries

Published online by Cambridge University Press:  14 August 2015

Geraldine J. Peters
Geraldine J. Peters*
Affiliation:
Department of Astronomy, University of Southern California, Los Angeles, CA 90007 USA

Extract

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At the last IAU Symposium on Be stars held in Bass River, MA in 1975, several of us (including P. Harmanec, M. Plavec, R.S. Polidan, and myself) suggested that Be stars are mass transfer binaries and represent the higher mass counterparts to the familiar Algol systems. Although a number of alternatives to the rotational hypothesis have been presented at this symposium (including “chromospheric” activity and non-radial pulsation) and some of these may well explain certain objects, I strongly believe that binary mass transfer is responsible (either directly or indirectly) for the circumstellar envelopes observed in a large percentage of Be stars.

Type
V. Rotation and Binarity
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 311 - 314
Copyright
Copyright © Reidel 1982 

References

Abt, H.A., Levy, S.G.: 1978, Astrophys. J. Suppl 36, pp. 241–258.CrossRefGoogle Scholar
Peters, G.J.: 1976, in Slettebak, A. (ed.), ‘Be and Shell Stars’, IAU Symp. 70, pp. 417–428.Google Scholar
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Peters, G.J., and Polidan, R.S.: 1982, this volume, pp. 405–409.Google Scholar
Plavec, M.: 1970, Publ. Astron. Soc. Pacific 82, pp. 957–995 Google Scholar
Poeckert, R.: 1981, Publ. Astron. Soc. Pacific 93, in press.Google Scholar
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Slettebak, A.: 1979, Space Science Reviews 23, pp. 541–580.Google Scholar