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.

Date of creation, presentation, or exhibit



AIPC 686 (2003) 201 "The Astrophysics of Gravitational Wave Sources": American Institute of Physics Conference Proceedings. Held at College Park, Maryland, 24-26 April 2003.||Also archived in: arXiv: astro-ph/0212270 v2 24 Aug 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. ISBN: 735401578Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type

Conference Proceeding

Department, Program, or Center

School of Physics and Astronomy (COS)


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