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Instability in Massive Stars: An Overview

Published online by Cambridge University Press:  04 August 2017

I. Appenzeller
I. Appenzeller*
Affiliation:
Landessternwarte, D-6900 Heidelberg, Federal Republic of Germany

Abstract

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Dynamical, vibrational, and thermal instabilities of massive blue stars are discussed as possible mechanisms for the observed brightness variations of such objects. Relaxation oscillations (on local thermal time scales) due to dynamical instabilities of the stellar wind flows appear to be the most likely mechanism, at least for the S Dor variables. Very massive main-sequence stars with M > 103 M⊙ should be violently vibrationally unstable and therefore should differ significantly from stable main-sequence stars of lower mass.

Type
Session 3. Luminous Blue Variables
Information
Symposium - International Astronomical Union , Volume 116: Luminous Stars and Associations in Galaxies , 1986 , pp. 139 - 149
Copyright
Copyright © Reidel 1986 

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