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Using a hydrodynamic adaptive mesh refinement code, we simulate the growthand evolution of a galaxy, which could potentially host a supermassive blackhole, within a cosmological volume. Reaching a dynamical range in excess of 10million, the simulation follows the evolution of the gas structure fromsuper-galactic 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 sub-pcscales. The gas density profile follows a power-law scaling as r^-8/3,consistent with an analytic description of turbulence in a quasi-stationarycircumnuclear disk. We analyze the properties of the disk which contribute tothe instabilities, and investigate the significance of instability for thegalaxy's evolution and the growth of a supermassive black hole at the center.

Resolving Gas Dynamics in the Circumnuclear Region of a Disk Galaxy in a Cosmological Simulation