Computer Science
Scientific paper
Oct 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001cqgra..18.3977l&link_type=abstract
Classical and Quantum Gravity, Volume 18, Issue 19, pp. 3977-3982 (2001).
Computer Science
4
Scientific paper
We have examined the dynamical evolution of dense stellar systems containing black holes that are formed by evolution of massive stars. The black holes, whose mass is approximately 10 Msolar, become the most massive component in a few times 107 yr. They quickly form a subsystem of very small size within the core of the cluster of ordinary stars via dynamical friction. The subsystem evolves on its own relaxation time scale, which is much shorter than the dynamical evolution time scale of the surrounding system. As the density of central parts of the black hole subsystem becomes large, the black holes form binaries, which eventually coalesce due to gravitational radiation. The repeated merger could lead to the formation of a `seed' black hole of mass around 1000 Msolar in the cluster centre if the velocity dispersion of the system is sufficiently large (i.e. >100 km s-1). The seed black hole can grow further by accreting surrounding gas.
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