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Radial and non-radial oscillations of spherically symmetric stellar systems

Published online by Cambridge University Press:  03 August 2017

Yousef Sobouti
Yousef Sobouti*
Affiliation:
Department of Physics and Biruni Observatory, Shiraz University, Shiraz, Iran

Abstract

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In an expansion scheme in velocity space, the first order perturbations of a stellar system bear close resemblance to those of a fluid. This feature is exploited to study the structure of the Hilbert space of the linear perturbations of a stellar system, to provide a classification for the modes, and to construct ansatz for variational calculations. The first order non-radial modes appear to be trispectral in that they are predominantly derived from a scalar potential, a toroidal vector potential, or a poloidal vector potential. The eigenfrequencies and the eigenfunctions of radial (ℓ = 0) and non-radial (ℓ, = 1) modes of polytropes and of truncated isothermal distributions are calculated. The density waves associated with these modes are also reported.

Type
Chapter 2: Theory of Solar Oscillations
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 191 - 194
Copyright
Copyright © Reidel 1988 

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