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.
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© 1988 International Astronomical Union
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Sobouti, Y. (1988). Radial and Non-Radial Oscillations of Spherically Symmetric Stellar Systems. In: Christensen-Dalsgaard, J., Frandsen, S. (eds) Advances in Helio- and Asteroseismology. International Astronomical Union / Union Astronomique Internationale, vol 123. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4009-3_43
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DOI: https://doi.org/10.1007/978-94-009-4009-3_43
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-277-2615-5
Online ISBN: 978-94-009-4009-3
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