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Brownian motion of black holes in stellar systems with non-Maxwellian distribution of the field stars

Published online by Cambridge University Press:  01 August 2006

Isabel Tamara Pedron  and
Carlos H. Coimbra-Araújo
Isabel Tamara Pedron
Affiliation:
Universidade Estadual do Oeste do Paraná, 85960-000, Marechal Cândido Rondon, PR, Brasil
Carlos H. Coimbra-Araújo
Affiliation:
Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-970, Campinas, SP, Brasil
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Abstract

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A massive black hole at the center of a dense stellar system, such as a globular cluster or a galactic nucleus, is subject to a random walk due gravitational encounters with nearby stars. It behaves as a Brownian particle, since it is much more massive than the surrounding stars and moves much more slowly than they do. If the distribution function for the stellar velocities is Maxwellian, there is a exact equipartition of kinetic energy between the black hole and the stars in the stationary state. However, if the distribution function deviates from a Maxwellian form, the strict equipartition cannot be achieved.

The deviation from equipartition is quantified in this work by applying the Tsallis q-distribution for the stellar velocities in a q-isothermal stellar system and in a generalized King model.

Keywords

black holesequipartitionTsallis distributionKing models
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 427 - 428
Copyright
Copyright © International Astronomical Union 2007

References

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Tsallis, C. 1988, J. Stat. Phys., 52, 479Google Scholar
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