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

Published online by Cambridge University Press:  01 September 2007

R. Spurzem ,
P. Berczik ,
I. Berentzen ,
D. Merritt ,
M. Preto  and
P. Amaro-Seoane
R. Spurzem
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie Univ. Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
P. Berczik
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie Univ. Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
I. Berentzen
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie Univ. Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
D. Merritt
Affiliation:
Dept. of Physics, 85 Lomb Memorial Drive, Rochester Institute of Technology, Rochester, NY14623-5604, USA
M. Preto
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie Univ. Heidelberg, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
P. Amaro-Seoane
Affiliation:
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476 Golm, Germany
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Abstract

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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.

Keywords

methods: numericaln-body simulationsgravitational wavesblack hole physicsgalaxies: star clustersnuclei
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S246: Dynamical Evolution of Dense Stellar Systems , September 2007 , pp. 346 - 350
Copyright
Copyright © International Astronomical Union 2008

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