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| Paper: |
Black Holes and Galaxy Evolution |
| Volume: |
197, XVth IAP Meeting Dynamics of Galaxies: From the Early Universe to the Present |
| Page: |
221 |
| Authors: |
Merritt, David |
| Abstract: |
Supermassive black holes appear to be generic components of galactic nuclei. Following their formation in the early universe, black holes should often find themselves in bound pairs as a consequence of galaxy mergers. The greatest uncertainty in estimating the coalescence time of black hole binaries is the degree to which a binary wanders about the center of the galactic potential. A simple model for binary decay is presented which qualitatively reproduces the evolution observed in the N-body simulations. The model predicts binary coalescence times that are never less than several billion years. Mass ejection by a decaying black hole binary should substantially lower the density of its host nucleus. The weak density cusps of bright ellipticals may be explained in this way if it is assumed that these galaxies formed from nearly gas-free mergers. |
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