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Dynamics of Black Holes in Rotating Cores

Published online by Cambridge University Press:  03 June 2010

Jose A. Fiestas  and
Rainer Spurzem
Jose A. Fiestas
Affiliation:
Zentrum für Astronomie, Univ. Heidelberg, Heidelberg, Germany Email: fiestas@ari.uni-heidelberg.de, spurzem@ari.uni-heidelberg.de
Rainer Spurzem
Affiliation:
Zentrum für Astronomie, Univ. Heidelberg, Heidelberg, Germany Email: fiestas@ari.uni-heidelberg.de, spurzem@ari.uni-heidelberg.de
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We study the dynamical interaction between stars surrounding black holes in self-gravitating galaxy cores by using realistic N-body techniques, calibrated by Fokker–Planck approximated models (Fiestas, Spurzem, & Kim 2006). We study the evolution over the relaxation time (collisional nuclei) of non-spherical (triaxial) models as flattening of the system due to rotation is allowed. We follow the interplay between velocity diffusion due to relaxation and black hole star accretion and study accretion rates and cusp formation in spherically symmetric and axisymmetric models.

Keywords

black hole physicskinematics and dynamicsgalaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S267: Co-Evolution of Central Black Holes and Galaxies , August 2009 , pp. 328
Copyright
Copyright © International Astronomical Union 2010

References

Fiestas, J., Spurzem, R., & Kim, E. 2006, MNRAS, 373, 677CrossRefGoogle Scholar
Fiestas, J., & Spurzem, R. 2010 [arXiv:0810.3800v1]Google Scholar