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Radial and Non-Radial Oscillations of Spherically Symmetric Stellar Systems

  • Yousef Sobouti
Conference paper
Part of the International Astronomical Union / Union Astronomique Internationale book series (IAUS, volume 123)

Abstract

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 = O) and non-radial (ℓ = l) modes of polytropes and of truncated isothermal distributions are calculated. The density waves associated with these modes are also reported.

Keywords

Stellar System Radial Mode Toroidal Field Standing Mode Isothermal Distribution 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© International Astronomical Union 1988

Authors and Affiliations

  • Yousef Sobouti
    • 1
  1. 1.Department of Physics and Biruni ObservatoryShiraz UniversityShirazIran

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