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Dynamics of Plane Stellar Systems

Published online by Cambridge University Press:  12 April 2016

Frank Hohl
Frank Hohl*
Affiliation:
NASA, Langley Research Center, Hampton, Virginia

Abstract

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The evolution of initially balanced rotating disks of stars is investigated with a computer model for isolated disks of stars. An isolated, initially cold balanced disk is found to be violently unstable. Adding a sufficient amount of velocity dispersion will stabilize all small-scale disturbances. However, the disks are still unstable against slowly growing long wave-length modes and after about two rotations most disks tend to assume a bar-shaped structure. It is found that the final mass distribution over most of the disk can be closely approximated by an exponential variation, irrespective of the initial mass distribution. The gravitational two-stream instability is investigated by means of a modified computer model for infinite doubly periodic stellar systems.

Information

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 10: Gravitational N-Body Problem , November 1971, pp. 91 - 109
Copyright
Copyright © Reidel 1971

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