Computer Science – Numerical Analysis
Scientific paper
Jun 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...427..793m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 427, no. 2, p. 793-807
Computer Science
Numerical Analysis
47
Binary Stars, Computerized Simulation, Galactic Clusters, Galactic Evolution, Globular Clusters, Many Body Problem, Star Clusters, Stellar Gravitation, Galactic Mass, Numerical Analysis, Star Distribution, Stellar Physics, Stellar Systems
Scientific paper
We present the results of N-body simulations of tidally limited star clusters with an initial population of 0%-20% binaries. We find that (1) if enough binaries are initially present, the binary fraction may fall to a minimum value, then increase at late times; (2) the cluster evaporation timescale is quite insensitive to the details of the initial binary distribution; (3) the cluster core radius stabilizes at a few percent of the half-mass radius when binaries are present, just as in the case of isolated clusters; and (4) there may be a marked difference between the spatial distribution of low-energy and high-energy binaries as the cluster evolves. Specifically, the spatial distribution of the lower energy systems is often substantially more extended than that of the more tightly bound pairs. At no time are our simulated clusters well described by simple dynamical models that neglect the close coupling between the binding energies and the center-of-mass energies of the binaries they contain.
Hut Piet
McMillan Steve
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