Dynamical evolution of star clusters in tidal fields

Baumgardt, H. and Makino, J. (2003) Dynamical evolution of star clusters in tidal fields. Monthly Notices of the Royal Astronomical Society, 340 1: 227-246. doi:10.1046/j.1365-8711.2003.06286.x


Author Baumgardt, H.
Makino, J.
Title Dynamical evolution of star clusters in tidal fields
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 0035-8711
1365-2966
Publication date 2003-03-01
Year available 2003
Sub-type Article (original research)
DOI 10.1046/j.1365-8711.2003.06286.x
Open Access Status DOI
Volume 340
Issue 1
Start page 227
End page 246
Total pages 20
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Language eng
Abstract We report the results of a large set of N-body calculations aimed at studying the evolution of multimass star clusters in external tidal fields. Our clusters start with the same initial mass functions, but varying particle numbers, orbital types and density profiles. Our main focus is to study how the stellar mass function and other cluster parameters change under the combined influence of stellar evolution, two-body relaxation and the external tidal field. We find that the lifetimes of star clusters moving on similar orbits scale as T similar toT(rh)(x), where T-rh is the relaxation time, and the exponent x depends on the initial concentration of the cluster and is around x approximate to 0.75. The scaling law does not change significantly if one goes from circular orbits to eccentric ones. From the results for the lifetimes, we predict that between 53 and 67 per cent of all Galactic globular clusters will be destroyed within the next Hubble time. Low-mass stars are preferentially lost and the depletion is strong enough to turn initially increasing mass functions into mass functions that decrease towards the low-mass end. The details of this depletion are insensitive to the starting condition of the cluster and can be characterized as a function of a single variable, such as, for example, the fraction of time spent until total cluster dissolution.
Keyword stellar dynamics
methods : N-body simulations
globular clusters : general
Initial Mass Function
Galactic Globular-Clusters
Monte-Carlo Simulations
N-Body Simulations
M-Circle-Dot
Stellar Evolution
Unequal Masses
Ccd Photometry
Main-Sequence
Black-Hole
Q-Index Code C1
Q-Index Status Provisional Code
Institutional Status Unknown

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