Journal Article

Monte Carlo simulations of star clusters — I. First Results

Mirek Giersz

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 298, issue 4, pages 1239-1248
Published in print August 1998 | ISSN: 0035-8711
Published online August 1998 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-8711.1998.01734.x
Monte Carlo simulations of star clusters — I. First Results

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Abstract

A revision of Stodoíkiewicz's Monte Carlo code is used to simulate evolution of star clusters. The new method treats each superstar as a single star and follows the evolution and motion of all individual stellar objects. The first calculations for isolated, equal-mass N-body systems with three-body energy generation according to Spitzer's formulae show good agreement with direct N-body calculations for N = 2000, 4096 and 10 000 particles. The density, velocity, mass distributions, energy generation, number of binaries, etc., follow the N-body results. Only the number of escapers is slightly too high compared with N-body results, and there is no level-off anisotropy for advanced post-collapse evolution of Monte Carlo models as is seen in N-body simulations for N ≤ 2000. For simulations with N > 10 000 gravothermal oscillations are clearly visible. The calculations of N 2000, 4096, 10 000, 32 000 and 100 000 models take about 2, 6, 20, 130 and 2500 h, respectively. The Monte Carlo code is at least 105 times faster than the N-body one for N = 32 768 with special-purpose hardware. Thus it becomes possible to run several different models to improve statistical quality of the data and run individual models with N as large as 100 000. The Monte Carlo scheme can be regarded as a method which lies in the middle between direct N-body and Fokker-Planck models and combines most advantages of both methods.

Keywords: methods: numerical; stars: kinematics; globular clusters: general

Journal Article.  0 words. 

Subjects: Astronomy and Astrophysics

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