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N-body simulations of interactions and mergings in small galaxy groups

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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In this paper I focus on three topics related to the dynamical evolution of small galaxy groups, for which the input of N-body simulations has been decisive. These are the merging rates in compact groups, the properties of remnants of multiple mergers, and the evolution of disc galaxies surrounded by one or more satellites. The short dynamical times of compact groups make it difficult to understand why such groups are observed at all. N-body simulations have pointed out two possible classes of solutions to this problem. The first one proposes that there is ongoing formation of compact groups, or that the longevity of the group is due to secondary infall. For the second class of solutions the longevity of compact groups is due either to their specific initial conditions, or to a massive common halo, encompassing the whole group. I discuss here these alternatives, together with their respective advantages and disadvantages. I then turn to the structure of remnants of multiple mergers and compare the results of N-body simulations with the properties of observed elliptical galaxies. Finally I discuss the dynamical evolution of a disc galaxy surrounded by one or more spherical satellites.

Type
Part 3. Numerical Simulations
Information
International Astronomical Union Colloquium , Volume 174: Small Galaxy Groups , 2000 , pp. 245 - 254
Copyright
Copyright © Astronomical Society of the Pacific 2000

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