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Non-Radial Oscillations

Published online by Cambridge University Press:  07 February 2017

P. Ledoux
P. Ledoux*
Affiliation:
Institut d'Astrophysique, Université de Liège, Belgium

Abstract

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The problem of the adiabatic non-radial oscillations of spherical stars is reviewed and results recalled for a variety of models. The anomalous behaviour of the eigenfunctions for highly condensed models is related to the apparent mobile singularities depending on the eigenvalues. Tables of Q-values are provided to facilitate possible applications to variable stars.

In the case of the gravity modes, the existence of multiple spectra some stable (g+ modes) some unstable (g− modes) if superadiabatic and subadiabatic regions alternate is discussed and the interest of further investigations underlined.

As far as vibrational stability (effects of the non adiabatic terms) is concerned, a general expression is given for the ‘damping coefficient’. The attention is drawn to the possibility for g+ modes of becoming vibrationally unstable under the effect of various factors and in various models, including the Sun where this was advocated as a possibility of relieving the neutrinos difficulty.

Finally the present status of the most obvious candidates among variable stars for non-radial oscillations, the β Canis Majoris stars and the rapid blue variables (white dwarfs) is briefly reviewed.

Type
Part VI Instability Mechanisms
Information
Symposium - International Astronomical Union , Volume 59: Stellar Instability and Evolution , 1974 , pp. 135 - 173
Copyright
Copyright © Reidel 1974 

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