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Formation and Evolution of Massive Black Holes in Star Clusters

Published online by Cambridge University Press:  30 March 2016

Holger Baumgardt ,
Junichiro Makino  and
Simon Portegies Zwart
Holger Baumgardt
Affiliation:
Institute of Advanced Physical and Chemical Research RIKEN, 2-1 Hirosawa, Wako-shi, Saitama 351-019, Japan
Junichiro Makino
Affiliation:
Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Simon Portegies Zwart
Affiliation:
Astronomical Institute “Anton Pannekoek” and Section Computational Science, University of Amsterdam, Kruislaan 403, 1098 SH Amsterdam, The Netherlands

Abstract

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We present results of N-body simulations on the formation of massive black holes by run-away merging in young star clusters and the later dynamical evolution of star clusters containing massive black holes. We determine the initial conditions necessary for run-away merging to form a massive black hole and study the equilibrium profile that is established in the cluster center as a result of the interaction of stars with the central black hole. Our results show that star clusters which contain black holes have projected luminosity profiles that can be fitted by standard King models. The presence of massive black holes in (post-)core collapse clusters is therefore ruled out by our simulations.

Type
I. Joint Discussions
Information
Highlights of Astronomy , Volume 13 , 2005 , pp. 350 - 353
Copyright
Copyright © Astronomical Society of Pacific 2005

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