  We demonstrate that the accretion disk model for the Galactic Center region
by Linden et al (1993a) is applicable for at least one order of magnitude in
radius from the Galactic Center (10 ... 100 pc). The viscosity $\nu$ is shown
to be weakly dependent on the radius $s$: $\nu \sim s^{0.4}$. Finally, we
discuss the influence of the inner boundary on the structure of the inner disk
regions.
