We numerically investigate dynamical evolution of a merger between a central massive black hole (MBH) and a gas clump with a mass of 106-107 M☉ in the central tens of parsecs of a galactic bulge. We found that the strong tidal gravitational field of the MBH transforms the initial spherical clump into a moderately thick gaseous disk (or torus) around the MBH. The developed disk is also found to show rotation, essentially because the tidal field changes efficiently the orbital angular momentum of the clump into intrinsic angular momentum of the disk. Furthermore, about a few percent of the gas mass (corresponding to a few 105 M☉) in the clump is found to be transferred to the central subparsec region around the MBH within an order of 106 yr. We thus suggest that successive merging of gas clumps onto an MBH can not only be associated closely with the formation of the nuclear disk around the MBH but also can provide gas fuel for the MBH.
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