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Global Instabilities of Disks∗

Published online by Cambridge University Press:  14 August 2015

J. M. Bardeen
J. M. Bardeen*
Affiliation:
Yale University, New Haven, Conn., U.S.A.

Abstract

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Current understanding of the stability of gas and stellar disks suggests very strongly that local stability to axisymmetric modes is not sufficient for global stability. A global instability to a bar mode will develop unless the rotational kinetic energy is sufficiently small compared with the random kinetic energy for the system as a whole. A disk as cool as the galactic disk near the Sun can survive only if most of the mass of the Galaxy is in a ‘hot’ component, such as a central bulge and/or an extended halo. We review the theoretical evidence for this conclusion coming from analytic results for simple gas and stellar disks, from numerical simulations of stellar disks, and from numerical calculations of the stability of gas disks. Some new results on the precise form of dynamic bar instabilities of gas disks with and without halos are reported.

Type
Part II/Flattened Systems
Information
Symposium - International Astronomical Union , Volume 69: Dynamics of Stellar Systems , 1975 , pp. 297 - 320
Copyright
Copyright © Reidel 1975 

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