  We discuss mechanisms for angular momentum transport in the clumpy medium of
the circumnuclear disk at the Galactic center. The viscosity due to clump-clump
collisions is found to be less than some critical viscosity; this meets the
conditions at which a collective mode of nonaxisymmetric shear perturbations in
the disk is able to grow until going into the saturation regime where fully
developed turbulence is established. We find that the angular momentum transfer
due to this turbulent viscosity turns out to comparable to the transport due to
magnetic torques. Taken together, the turbulent and magnetic transfer of
angular momentum are able to provide the inflow of mass into the central parsec
with a rate of about 10^{-2} M_{sun}/yr, consistent with the available data.
