The main sequence of star clusters

Kupper, Andreas H. W., Kroupa, Pavel and Baumgardt, Holger (2008) The main sequence of star clusters. Monthly Notices of the Royal Astronomical Society, 389 2: 889-902. doi:10.1111/j.1365-2966.2008.13598.x


Author Kupper, Andreas H. W.
Kroupa, Pavel
Baumgardt, Holger
Title The main sequence 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 2008-09
Sub-type Article (original research)
DOI 10.1111/j.1365-2966.2008.13598.x
Open Access Status DOI
Volume 389
Issue 2
Start page 889
End page 902
Total pages 14
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Language eng
Formatted abstract
A novel way of looking at the evolution of star clusters is presented here. With a dynamical temperature, given by the mean kinetic energy of the cluster stars, and a dynamical luminosity, which is defined as the kinetic energy of the stars leaving the cluster in analogy to the energy of photons emitted by a star, the dissolution of star clusters is studied using a new dynamical temperature–luminosity diagram for star clusters. The investigation contains a parameter-space study of open clusters of up to N = 32 768 single-mass stars with different initial density distributions, half-mass radii, tidal conditions and binary fractions. The clusters show a strong correlation between dynamical temperature and dynamical luminosity and most of the investigated cluster families share a common sequence in such a dynamical temperature–luminosity diagram. Deviations from this sequence are analysed and discussed. After core collapse, the position of a cluster within this diagram can be defined by three parameters: the mass; the tidal conditions and the binary fraction. Due to core collapse all initial conditions are lost and the remaining stars adjust to the given tidal conditions. Binaries as internal energy sources influence this adjustment. A further finding concerns the Lagrange radii of star clusters: Throughout the investigated parameter space nearly all clusters show a constant half-mass radius for the time after core collapse until dissolution. Furthermore, the ratio of half-mass radius to tidal radius evolves on to a common sequence which only depends on the mass left in the cluster.
Keyword Stellar dynamics
methods : N-body simulations
Hertzsprung-Russel (HR) diagram
Open clusters and assoziations : general
Q-Index Code C1
Q-Index Status Provisional Code
Institutional Status Non-UQ

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