Radial and nonradial stability of spherical stellar systems

Details Radial and nonradial stability of spherical stellar systems Radial and nonradial stability of spherical stellar systems

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328...93d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 1, 1988, p. 93-102.

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28

Elliptical Galaxies, Galactic Evolution, Galactic Structure, Radial Velocity, Stellar Motions, Stellar Systems, Astronomical Models, Circular Orbits, Computational Astrophysics, Density Distribution, Perturbation Theory

Scientific paper

The stability to radial and nonradial perturbations of an extensive set of stellar dynamical models with the Plummer density law is investigated. Radial stability of a large subset of the models can be demonstrated using either a generalization of Antonov's (1962) sufficient criterion for isotropic systems, or a very simple criterion by Doremus and Feix (1973). Nonradial stability, and radial stability of models not satisfying Antonov's criterion, are tested with a mean-field N-body code. It is found that models near the limit of maximum radial velocity anisotropy are unstable to the formation of a bar. Models composed of nearly circular orbits are apparently stable. Of the three types of instability studied by Barnes, Goodman, and Hut (1985) in a family of generalized polytropes, only one, the 'radial-orbit instability', is active in these models. It is argued that the same is likely to be true in any family of spherical models with a density profile similar to those of real stellar systems.

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