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Growing Supermassive Black Holes Inside Cosmological Simulations

Published online by Cambridge University Press:  03 June 2010

Robyn Levine ,
Nickolay Y. Gnedin  and
Andrew J. S. Hamilton
Robyn Levine
Affiliation:
Canadian Institute for Theoretical Astrophysics, Toronto, ON M5S 3H8, Canada
Nickolay Y. Gnedin
Affiliation:
Fermi National Accelerator Laboratory, Batavia, IL 60510, USA
Andrew J. S. Hamilton
Affiliation:
University of Colorado, Boulder, CO 80309, USA
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Using a hydrodynamic adaptive mesh refinement code, we simulate the growth and evolution of a typical disk galaxy hosting a supermassive black hole (SMBH) within a cosmological volume. The simulation covers a dynamical range of 10 million, which allows us to study the transport of matter and angular momentum from super-galactic scales down to the outer edge of the accretion disk around the SMBH. A dynamically interesting circumnuclear disk develops in the central few hundred parsecs of the simulated galaxy, through which gas is stochastically transported to the central black hole.

Keywords

galaxies: evolutiongalaxies: high-redshiftgalaxies: nuclei
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. 333
Copyright
Copyright © International Astronomical Union 2010

References

Kravtsov, A. V., Klypin, A., & Hoffman, Y. 2002, ApJ, 571, 563Google Scholar
Levine, R., Gnedin, N. Y., Hamilton, A. J. S., & Kravtsov, A. V. 2008, ApJ, 678, 154CrossRefGoogle Scholar