The Physics of Supermassive Black Hole Mergers

Details The Physics of Supermassive Black Hole Mergers The Physics of Supermassive Black Hole Mergers

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..apr.l9004m&link_type=abstract

American Physical Society, April Meeting, 2004, May 1-4, 2004, Denver, Colorado April 2004, MEETING ID: APR04, abstract #L9.004

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The coalescence of supermassive black hole binaries is one of the main sources of low-frequency gravitational radiation that will be detected by space-based gravitational wave observatories. All luminous galaxies appear to contain black holes in their centers. When two or more galaxies merge, a binary may form at the center of the new galaxy. The fate of the binary system depends on its interaction with the environment. In a galactic nucleus the black hole is embedded in a concentration of interstellar gas and stars. A variety of processes can drive the black holes to coalescence. I review recent progress in the study of these processes. I also review the arguments for the ubiquity of supermassive black hole mergers in the universe, and discuss cosmological implications of the expected detection of gravitational waves from these sources.

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