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6.1. Non-axisymmetric dynamics in galaxy centers

Published online by Cambridge University Press:  25 May 2016

F. Combes
F. Combes*
Affiliation:
Observatoire de Paris, DEMIRM, 61 Av. de l'Observatoire, F-75 014 Paris, France

Abstract

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Our Galaxy is representative of the majority of spiral galaxies, which are highly non-axisymmetric, developping bars (m = 2 perturbations), but also lopsidedness and off-centering (m = 1), and superposed higher order perturbations. Recent high-resolution N-body and gas-dynamical simulations have considerably improved our knowledge on the nature and formation of these features. Contrary to previous beliefs, they are not long-lived, but fade away and can be reformed continuously, provided enough gas is supplied to the center, to maintain gravitational instability. The dynamical mechanisms involved are reviewed and discussed, and in particular the new features brought by the dissipative gas component. The role of these axisymmetries in the galaxy evolution, mass concentration, together with nucleus fueling are described, and typical time-scales discussed in particular for confrontation to the Milky Way observations.

Type
Part II. Nuclear Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 257 - 264
Copyright
Copyright © Kluwer 1998 

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