Growth of Intermediate-Mass Black Holes in Globular Clusters

Details Growth of Intermediate-Mass Black Holes in Globular Clusters Growth of Intermediate-Mass Black Holes in Globular Clusters

2004-02-23

arxiv.org/abs/astro-ph/0402532v1

Astrophys.J. 616 (2004) 221-230

Astronomy and Astrophysics

Astrophysics

28 pages including 9 figures, submitted to ApJ

Scientific paper

10.1086/424809

We present results of numerical simulations of sequences of binary-single scattering events of black holes in dense stellar environments. The simulations cover a wide range of mass ratios from equal mass objects to 1000:10:10 solar masses and compare purely Newtonian simulations to simulations in which Newtonian encounters are interspersed with gravitational wave emission from the binary. In both cases, the sequence is terminated when the binary's merger time due to gravitational radiation is less than the arrival time of the next interloper. We find that black hole binaries typically merge with a very high eccentricity (0.93 < e < 0.95 pure Newtonian; 0.85 < e < 0.90 with gravitational wave emission) and that adding gravitational wave emission decreases the time to harden a binary until merger by ~ 30% to 40%. We discuss the implications of this work for the formation of intermediate-mass black holes and gravitational wave detection.

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