Space-based observations are beginning to yield detailed information about the stellar kinematics at the very centers of galaxies, within the sphere of gravitational influence of the black hole. The structure and dynamics of these regions is probably determined in part by the infall and coalescence of black holes during galaxy mergers. A goal of N-body simulations is to reproduce the kinematics near the black holes as well as the relations that exist between the nuclear and global properties of galaxies. However, the problem is computationally difficult due to the wide range of length and time scales, and no single N-body code can efficiently follow the evolution from kiloparsec to sub-parsec scales. We review existing N-body work on this problem and present the first, fully self-consistent merger simulations of galaxies containing dense stellar cusps and black holes.

Date of creation, presentation, or exhibit



ASP Conference Series Vol. 228, Issue: Dynamics of Star Clusters and the Milky Way, 2001 p.155 Proceedings of the Astronomical Society of the Pacific Conference Series, Pasadena, California 2000||Also archived in: arXiv:astro-ph/0008497 v1 30 Aug 2000 AND Rutgers Astrophysics Preprint Series No. 277 This work was supported by NASA through grant NAG5-6037 and by the NSF through grant AST 96-17088. ISBN: 1-58381-060-9Note: 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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