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Generation of Oscillatory Motions in the Stellar Atmosphere

Published online by Cambridge University Press:  12 April 2016

Yoji Osaki
Yoji Osaki*
Affiliation:
Department of Astronomy, University of Tokyo, Tokyo, Japan

Abstract

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Thermal overstability of non-radial eigenmodes of stars is discussed as one of possible causes for generating non-thermal motions in the stellar atmosphere. The nature of oscillatory motions in stars is first considered both in the local and the global stand points. Then, the excitation of eigen-oscillations is discussed and results of numerical studies so far made are reviewed for the vibrational stability of various stellar models against non-radial oscillations. It is found that many of non-radial p-modes of high tesseral harmonics are likely excited in various stars of the HR diagram and that they possibly manifest themselves as non-thermal velocity fields in the stellar atmosphere.

Type
1. The Pyhsical Origin of Turbulence
Information
International Astronomical Union Colloquium , Volume 51: Stellar Turbulence , 1980 , pp. 38 - 50
Copyright
Copyright © Springer-Verlag 1980

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