Published October 15, 2003
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The Final Parsec Problem
- Creators
- Milosavljević, Miloš
- Merritt, David
- Others:
- Centrella, Joan M.
- Barnes, Sandy
Abstract
The coalescence of massive black hole binaries is one of the main sources of low-frequency gravitational radiation that can be detected by LISA. When two galaxies containing massive black holes merge, a binary forms at the center of the new galaxy. We discuss the evolution of the binary after its separation decreases below one parsec. Whether or not stellar dynamical processes can drive the black holes to coalesce depends on the supply of stars that scatter against the binary. We discuss various mechanisms by which this supply can be replenished after the loss cone has been depleted.
Additional Information
©2003 American Institute of Physics. Issue Date: October 15, 2003. This work was supported by NSF grants AST 00-71099 and by NASA grants NAG5-6037 and NAG5-9046 to DM, and by a Sherman Fairchild Postdoctoral Fellowship to MM.Files
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Additional details
- Eprint ID
- 9599
- Resolver ID
- CaltechAUTHORS:MILaipcp03
- Created
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2008-02-12Created from EPrint's datestamp field
- Updated
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2021-11-08Created from EPrint's last_modified field
- Series Name
- American Institute of Physics Conference Proceedings
- Series Volume or Issue Number
- 686