Formation and Evolution of Black Holes in Galactic Nuclei and Star Clusters

Details Formation and Evolution of Black Holes in Galactic Nuclei and Star Clusters Formation and Evolution of Black Holes in Galactic Nuclei and Star Clusters

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..246..346s&link_type=abstract

Dynamical Evolution of Dense Stellar Systems, Proceedings of the International Astronomical Union, IAU Symposium, Volume 246, p.

Physics

Methods: Numerical, N-Body Simulations, Gravitational Waves, Black Hole Physics, Galaxies: Star Clusters, Nuclei

Scientific paper

We study the formation, growth, and co-evolution of single and multiple supermassive black holes (SMBHs) and compact objects like neutron stars, white dwarfs, and stellar mass black holes in galactic nuclei and star clusters, focusing on the role of stellar dynamics. In this paper we focus on one exemplary topic out of a wider range of work done, the study of orbital parameters of binary black holes in galactic nuclei (binding energy, eccentricity, relativistic coalescence) as a function of initial parameters. In some cases the classical evolution of black hole binaries in dense stellar systems drives them to surprisingly high eccentricities, which is very exciting for the emission of gravitational waves and relativistic orbit shrinkage. Such results are interesting to the emerging field of gravitational wave astronomy, in relation to a number of ground and space based instruments designed to measure gravitational waves from astrophysical sources (VIRGO, Geo600, LIGO, LISA). Our models self-consistently cover the entire range from Newtonian dynamics to the relativistic coalescence of SMBH binaries.

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