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Phase changes in Be stars: The Be-shell and Be phases of Pleione

Published online by Cambridge University Press:  26 May 2016

V. Doazan ,
A. de La Fuente ,
N. Cramer  and
M. Barylak
V. Doazan
Affiliation:
Observatoire de Paris, 61, Av. de l'Observatoire, F-75014 Paris
A. de La Fuente
Affiliation:
INSA-VILSPA, Apartado 50727, E-28080 Madrid
N. Cramer
Affiliation:
Observatoire de Genève, CH-1290 Sauverny, Suisse
M. Barylak
Affiliation:
ESA IUE Observatory, Apartado 50727, E-28080 Madrid

Extract

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Phase changes from Be to Be-shell and/or B normal, and conversely, presently remain unpredictable in Be stars (except in some binaries where the transition to a shell phase seems to be associated with the orbital period). Because of their unpredictable character, these phenomena have been monitored in very few cases and are still very poorly understood. However, the existence of phase transitions have strong modelling implications. Under the disk model, the inclination of the star's rotation axis determines the type of spectrum, Be or Be-shell, that a given Be star may exhibit. It is obvious that this picture is contradicted by phase transitions (Doazan 1982).

Type
6. Be Stars: Circumstellar Environment
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 360 - 361
Copyright
Copyright © Kluwer 1994 

References

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Doazan, V., de la Fuente, A., Barylak, M., Cramer, N., 1993a, in Weiss, W. W., Baglin, A., (eds), Inside the stars , IAU Colloq. 137, p 787 CrossRefGoogle Scholar
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