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Evolution of Bars in Isolated and in Interacting Disk Galaxies

Published online by Cambridge University Press:  12 April 2016

E. Athanassoula
E. Athanassoula*
Affiliation:
Observatoire de Marseille, 2 Place Le Verrier, 13248 Marseille Cedex 04, France

Abstract

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I use N-body simulations to follow the evolution of bars in both isolated and interacting disk galaxies. The pattern speeds of bars evolving in isolated galaxies decline gradually with time, due to transfer of angular momentum from the bar to other components in the galaxy. Both the form and amount of this decline depend on the model used. The fate of a bar in an interacting disk galaxy depends on the mass, central concentration and orbit of the perturber. The pattern speed, form and amplitude of the bar may change, the bar can become off-centered, or, more drastically, it can disappear altogether. Finally I propose a scenario for the evolution of NGC 7217, which could, if proven correct, explain the formation of the rings in that galaxy and also, at least qualitatively, the existence of a retrograde population.

Type
Part VI. Theory of Barred Galaxies II.
Information
International Astronomical Union Colloquium , Volume 157: Barred Galaxies , 1996 , pp. 309 - 320
Copyright
Copyright © Astronomical Society of the Pacific 1996

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