MOCCA code for star cluster simulations - III. Stellar-mass black holes in the globular cluster M22

被引:36
作者
Heggie, Douglas C. [1 ,2 ]
Giersz, Mirek [3 ]
机构
[1] Univ Edinburgh, Sch Math, Edinburgh EH9 3JZ, Midlothian, Scotland
[2] Univ Edinburgh, Maxwell Inst Math Sci, Edinburgh EH9 3JZ, Midlothian, Scotland
[3] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland
关键词
methods: numerical; globular clusters: individual: NGC 6656; MONTE-CARLO SIMULATIONS; DYNAMICAL EVOLUTION; MILKY-WAY; BINARY; CORE; RETENTION; PROFILES; CATALOG; MERGERS; RATES;
D O I
10.1093/mnras/stu102
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Using a Monte Carlo code, we construct a dynamic evolutionary model of the Galactic globular cluster M22 (NGC 6656). The initial conditions are chosen so that, after about 12 Gyr of stellar and dynamical evolution, the model is an approximate fit to the surface brightness and velocity dispersion profiles of the cluster, to its mass function and to the current binary fraction. Depending on the distribution of black hole natal kicks, we predict that the present-day population of stellar-mass black holes ranges from about 40 (no kicks) down to essentially zero (kicks distributed like those of neutron stars). Provided that natal kicks do not eject all new black holes, it is suggested that clusters with a present-day half-mass relaxation time above about 1 Gyr are the ones that may still retain an appreciable population of black holes.
引用
收藏
页码:2459 / 2467
页数:9
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