Other
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..apr.c5003m&link_type=abstract
American Physical Society, April Meeting, 2003, April 5-8, 2003 Philadelphia, Pennsylvania, MEETING ID: APR03, abstract #C5.003
Other
Scientific paper
Mergers of stellar-mass black-hole binaries can release large amounts of gravitational radiation in the ˜100 Hz range, making them attractive LIGO targets. However, conventional binary evolution models generally predict merger rates too low to be of observational interest. An alternative possibility is that black holes instead become members of close binaries through dynamical interactions in dense star clusters. The black-hole binaries become tightly bound via superelastic encounters with other cluster members, and are ultimately ejected from their parent cluster. N-body simulations suggest that a significant fraction of escaping black-hole binaries may have orbital periods short enough and eccentricities high enough that the emission of gravitational radiation causes them to coalesce within a few billion years. We predict a black-hole merger rate of approximately 3 × 10-7 per year per cubic megaparsec, although the numbers are uncertain as they depend sensitively on cluster parameters. This merger rate implies one or two LIGO detections during the first two years of operation. For the advanced detector, the detection rate rises to roughly 1 per day.
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