Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21540416b&link_type=abstract
American Astronomical Society, AAS Meeting #215, #404.16; Bulletin of the American Astronomical Society, Vol. 42, p.227
Astronomy and Astrophysics
Astronomy
Scientific paper
Shortly after a galaxy merger, the supermassive black holes from each galaxy are thought to form a binary at the center of the merger remnant. The binary orbit shrinks via three-body scattering of stars until the black holes are close enough to strongly emit gravitational radiation and merge. Since a substantial fraction of the scattered stars are ejected with enough energy to escape the host galaxy, three-body encounters with a supermassive binary black hole are a viable mechanism to generate hypervelocity stars. We investigate the 3-d spatial and kinematic distribution of the stars that are scattered by interacting with a supermassive binary black hole. We simulate each three body encounter explicitly, including gravitational radiation, until the stellar interloper has either been ejected or has merged with a black hole. Then, we evolve the positions and velocities of the scattered stars self-consistently within an N-body galactic model. By mapping the motion of these scattered stars as they traverse the galactic potential, we can characterize their distribution and how it evolves with time. We discuss how the anisotropic distribution of the scattered stars could allow us to determine characteristics of the black hole binary, as well as aid in the search for hypervelocity stars.
Benson Amanda
Gultekin Kayhan
Holley-Bockelmann Kelly
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