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Non-radially Pulsating Hot Stars: Non-radial Pulsations and Be Phenomenon

Published online by Cambridge University Press:  12 April 2016

Yoji Osaki
Yoji Osaki*
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo, 113, Japan

Abstract

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We discuss a possible role of non-radial oscillations as a cause of mass-loss in hot stars. In particular, we propose a working model for the episodic mass-loss in Be stars. In this model, equatorial mass loss is thought to be driven by wave-breaking phenomenon of large-amplitude non-radial waves and a circumstellar disk could thus be formed around the equatorial plane of a rapidly rotating star. A kind of relaxation-oscillation cycle could be established between the Be phase and non-Be phase, in which an interplay between non-radial oscillations in stellar atmosphere and the circumstellar disk is essential. We also discuss a viscous decretion-disk model for the circumstellar envelope around Be stars.

Type
Section V Pulsation
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 329 - 336
Copyright
Copyright © Springer-Verlag 1999

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