Mass-loss rates and the mass evolution of star clusters

Lamers, Henny J. G. L. M., Baumgardt, Holger and Gieles, Mark (2010) Mass-loss rates and the mass evolution of star clusters. Monthly Notices of the Royal Astronomical Society, 409 1: 305-328. doi:10.1111/j.1365-2966.2010.17309.x


Author Lamers, Henny J. G. L. M.
Baumgardt, Holger
Gieles, Mark
Title Mass-loss rates and the mass evolution of star clusters
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 0035-8711
1365-2966
Publication date 2010-11
Sub-type Article (original research)
DOI 10.1111/j.1365-2966.2010.17309.x
Open Access Status DOI
Volume 409
Issue 1
Start page 305
End page 328
Total pages 24
Place of publication Oxford, United Kindom
Publisher Oxford University Press
Collection year 2011
Language eng
Formatted abstract
We describe the interplay between stellar evolution and dynamical mass loss of evolving star clusters, based on the principles of stellar evolution and cluster dynamics and on the details of a grid of N-body simulations of Galactic cluster models. The cluster models have different initial masses, different orbits, including elliptical ones, and different initial density profiles. We use two sets of cluster models: one set of Roche lobe filling models and a new set of cluster models that are initially underfilling their tidal radius.

We identify four distinct mass-loss effects: (1) mass loss by stellar evolution, (2) loss of stars induced by stellar evolution and (3) relaxation-driven mass loss before and (4) after core collapse. At young ages the mass loss is dominated by stellar evolution, followed by the evolution-induced loss of stars. This evolution-induced mass loss is important if a cluster is immersed in the tidal field. Both the evolution-induced loss of stars and the relaxation-driven mass loss need time to build up. This is described by a delay function that has a characteristic time-scale of a few crossing times for Roche lobe filling clusters and a few half-mass relaxation times for initially Roche lobe underfilling clusters. The relaxation-driven mass loss (called ‘dissolution’ in this paper) can be described by a simple power-law dependence of the mass d(M/M⊙)/dt=−(M/M⊙)1 −γ/t0, where t0 depends on the orbit and environment of the cluster. The index γ is 0.65 for clusters with a King parameter W0= 5 for the initial density distribution, and 0.80 for more concentrated clusters with W0= 7. For initially Roche lobe underfilling clusters the dissolution is described by the same γ= 0.80, independent of the initial density distribution. The values of the constant t0 are derived for the models and described by simple formulae that depend on the orbit of the cluster. The mass-loss rate increases by about a factor of 2 at core collapse and the mass dependence of the relaxation-driven mass loss changes to γ= 0.70 after core collapse.

We also present a simple recipe for predicting the mass evolution of individual star clusters with various metallicities and in different environments, with an accuracy of a few per cent in most cases. This can be used to predict the mass evolution of cluster systems.
Copyright © 1999-2010 John Wiley & Sons, Inc. All Rights Reserved.
Keyword Galaxy: general
Globular clusters: general
Galaxy: halo
Galaxies: star clusters: general
Q-Index Code C1
Q-Index Status Confirmed Code
Institutional Status UQ
Additional Notes Published under Papers.

Document type: Journal Article
Sub-type: Article (original research)
Collections: School of Mathematics and Physics
Official 2011 Collection
 
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Citation counts: TR Web of Science Citation Count  Cited 42 times in Thomson Reuters Web of Science Article | Citations
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Created: Sun, 12 Dec 2010, 00:02:42 EST