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Title:
A comprehensive set of simulations studying the influence of gas expulsion on star cluster evolution
Authors:
Baumgardt, H.; Kroupa, P.
Affiliation:
AA(Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany; ), AB(Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany; )
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 380, Issue 4, pp. 1589-1598. (MNRAS Homepage)
Publication Date:
10/2007
Origin:
MNRAS
MNRAS Keywords:
stellar dynamics , methods: N-body simulations , stars: formation , open clusters and associations: general , galaxies: star clusters
Abstract Copyright:
(c) 2007 The Authors. Journal compilation © 2007 RAS
DOI:
10.1111/j.1365-2966.2007.12209.x
Bibliographic Code:
2007MNRAS.380.1589B

Abstract

We have carried out a large set of N-body simulations studying the effect of residual-gas expulsion on the survival rate, and final properties of star clusters. We have varied the star formation efficiency (SFE), gas expulsion time-scale and strength of the external tidal field, obtaining a three-dimensional grid of models which can be used to predict the evolution of individual star clusters or whole star cluster systems by interpolating between our runs. The complete data of these simulations are made available on the internet.

Our simulations show that cluster sizes, bound mass fraction and velocity profile are strongly influenced by the details of the gas expulsion. Although star clusters can survive SFEs as low as 10 per cent if the tidal field is weak and the gas is removed only slowly, our simulations indicate that most star clusters are destroyed or suffer dramatic loss of stars during the gas removal phase. Surviving clusters have typically expanded by a factor of 3 or 4 due to gas removal, implying that star clusters formed more concentrated than as we see them today. Maximum expansion factors seen in our runs are around 10. If gas is removed on time-scales smaller than the initial crossing time, star clusters acquire strongly radially anisotropic velocity dispersions outside their half-mass radii. Observed velocity profiles of star clusters can therefore be used as a constraint on the physics of cluster formation.

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