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The Galactic center stellar disk and the circumnuclear ring provide a uniqueopportunity to study in detail the dynamics and physical conditions of distantmolecular disks in the nuclei of galaxies. One of the key questions is howthese disks form so close to their host black holes and under what conditionthey form stars in a tidally stressed environment. We argue that disk formationaround a massive black hole is due to partial accretion of extended molecularclouds that temporarily pass through the central region of the Galaxy. Thecancellation of angular momentum of the gravitationally focused gas naturallycreates a compact gaseous disk. The disk can potentially become gravitationallyunstable and form stars. We apply these ideas to explain the origin ofsub-parsec megamaser disks found in the nuclei of Seyfert 2 galaxies. We showthat an empirical scaling relation between the mass of the black hole and thesize of the disk can be understood in the context of the cloud capturescenario. We conclude that the stellar and gas disks found in our Galacticcenter act as a bridge to further our understanding of more distant mega-maserdisks in the nuclei of Seyfert 2 galaxies.

The Origin of Parsec-Scale Gaseous and Stellar Disks in the Galactic Center and AGNs