A prescription and fast code for the long-term evolution of star clusters - III. Unequal masses and stellar evolution

Alexander, Poul E. R., Gieles, Mark, Lamers, Henny J. G. L. M. and Baumgardt, Holger (2014) A prescription and fast code for the long-term evolution of star clusters - III. Unequal masses and stellar evolution. Monthly Notices of the Royal Astronomical Society, 442 2: 1265-1285. doi:10.1093/mnras/stu899

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Author Alexander, Poul E. R.
Gieles, Mark
Lamers, Henny J. G. L. M.
Baumgardt, Holger
Title A prescription and fast code for the long-term evolution of star clusters - III. Unequal masses and stellar evolution
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 0035-8711
1365-2966
Publication date 2014-08-01
Year available 2014
Sub-type Article (original research)
DOI 10.1093/mnras/stu899
Open Access Status File (Publisher version)
Volume 442
Issue 2
Start page 1265
End page 1285
Total pages 21
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Language eng
Abstract We present a new version of the fast star cluster evolution code Evolve Me A Cluster of StarS (emacss). While previous versions of emacss reproduced clusters of single-mass stars, this version models clusters with an evolving stellar content. Stellar evolution dominates early evolution, and leads to: (1) reduction of the mean mass of stars due to the mass loss of high-mass stars; (2) expansion of the half-mass radius; (3) for (nearly) Roche Volume filling clusters, the induced escape of stars. Once sufficient relaxation has occurred (a parts per thousand integral 10 relaxation times-scales), clusters reach a second, 'balanced' state whereby the core releases energy as required by the cluster as a whole. In this state: (1) stars escape due to tidal effects faster than before balanced evolution; (2) the half-mass radius expands or contracts depending on the Roche volume filling factor; and (3) the mean mass of stars increases due to the preferential ejection of low-mass stars. We compare the emacss results of several cluster properties against N-body simulations of clusters spanning a range of initial number of stars, mass, half-mass radius, and tidal environments, and show that our prescription accurately predicts cluster evolution for this data base. Finally, we consider applications for emacss, such as studies of galactic globular cluster populations in cosmological simulations.
Keyword N-Body Simulations
Monte-Carlo Simulations
Globular-Clusters
Black-Holes
Dynamical Evolution
Tidal Fields
Adiabatic Invariants
Core-Collapse
Milky-Way
Systems
Q-Index Code C1
Q-Index Status Provisional Code
Grant ID FT0991052
Institutional Status UQ
Additional Notes This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 The Authors Monthly Notices of the Royal Astronomical Society. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Document type: Journal Article
Sub-type: Article (original research)
Collection: School of Mathematics and Physics
 
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