paper

A stochastic Monte Carlo approach to model real star cluster evolution, II. Self-consistent models and primordial binaries

arXiv:astro-ph/9911504 · doi:10.1046/j.1365-8711.2000.03727.x

Abstract

The new approach outlined in Paper I (Spurzem \& Giersz 1996) to follow the individual formation and evolution of binaries in an evolving, equal point-mass star cluster is extended for the self-consistent treatment of relaxation and close three- and four-body encounters for many binaries (typically a few percent of the initial number of stars in the cluster). The distribution of single stars is treated as a conducting gas sphere with a standard anisotropic gaseous model. A Monte Carlo technique is used to model the motion of binaries, their formation and subsequent hardening by close encounters, and their relaxation (dynamical friction) with single stars and other binaries. The results are a further approach towards a realistic model of globular clusters with primordial binaries without using special hardware. We present, as our main result, the self-consistent evolution of a cluster consisting of 300.000 equal point-mass stars, plus 30.000 equal mass binaries over several hundred half-mass relaxation times, well into the phase where most of the binaries have been dissolved and evacuated from the core. In a self-consistent model it is the first time that such a realistically large number of binaries is evolving in a cluster with an even ten times larger number of single stars. Due to the Monte Carlo treatment of the binaries we can at every moment analyze their external and internal parameters in the cluster as in an N-body simulation.

LaTeX MNRAS Style 21 pages, 34 figures, submitted to MNRAS Nov. 1999, for preprint, see ftp://ftp.ari.uni-heidelberg.de/pub/spurzem/warspaper-98.ps.gz for associated mpeg-files (20 MB and 13 MB, respectively), see ftp://ftp.ari.uni-heidelberg.de/pub/spurzem/movie1.mpg and ftp://ftp.ari.uni-heidelberg.de/pub/spurzem/movie2.mpg

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