Issue |
A&A
Volume 372, Number 1, June II 2001
|
|
---|---|---|
Page(s) | 105 - 116 | |
Section | Galactic structure, stellar clusters, and populations | |
DOI | https://doi.org/10.1051/0004-6361:20010477 | |
Published online | 15 June 2001 |
The mean surface density of companions in a stellar-dynamical context
1
UCO/Lick Observatory, University of California, 499 Kerr Hall, Santa Cruz, CA 95064, USA
2
Otto Hahn Fellow, Max-Planck-Institut für Astronomie, Königstuhl 17, 69917 Heidelberg, Germany
3
Sterrewacht Leiden, Postbus 9513, 2300-RA Leiden, The Netherlands
4
Institut für Theoretische Physik und Astrophysik, Universität Kiel, 24098 Kiel, Germany e-mail: pavel@astrophysik.uni-kiel.de
Corresponding author: R. S. Klessen, ralf@ucolick.org
Received:
11
July
2000
Accepted:
26
March
2001
Applying the mean surface density of companions, , to the
dynamical evolution of star clusters is an interesting approach to
quantifying structural changes in a cluster. It has the advantage
that the entire density structure, ranging from the closest binary
separations, over the core-halo structure through to the density
distribution in moving groups that originate from clusters, can be
analysed coherently as one function of the stellar separation r. This contribution assesses the evolution of
for clusters
with different initial densities and binary populations. The changes
in the binary, cluster and halo branches as the clusters evolve are
documented using direct N-body calculations, and are correlated with
the cluster core and half-mass radius. The location of breaks in the
slope of
and the possible occurrence of a binary gap can
be used to infer dynamical cluster properties.
Key words: stars: binaries: general / open clusters and associations: general / stars: formation / stellar dynamics
© ESO, 2001
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