Journal
ASTROPHYSICAL JOURNAL
Volume 678, Issue 1, Pages 154-167Publisher
UNIV CHICAGO PRESS
DOI: 10.1086/529064
Keywords
galaxies : evolution; galaxies : high-redshift; galaxies : ISM; galaxies : nuclei; galaxies : structure
Categories
Ask authors/readers for more resources
Using a hydrodynamic adaptive mesh refinement code, we simulate the growth and evolution of a galaxy, which could potentially host a supermassive black hole, within a cosmological volume. Reaching a dynamical range in excess of 10 million, the simulation follows the evolution of the gas structure from supergalactic scales all the way down to the outer edge of the accretion disk. Here we focus on global instabilities in the self- gravitating, cold, turbulence-supported, molecular gas disk at the center of the model galaxy, which provide a natural mechanism for angular momentum transport down to subparsec scales. The gas density profile follows a power law alpha r(-8/3), consistent with an analytic description of turbulence in a quasi- stationary circumnuclear disk. We analyze the properties of the disk which contribute to the instabilities and investigate the significance of instability for the galaxy's evolution and the growth of a supermassive black hole at the center.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available