We demonstrate that the accretion disk model for the Galactic Center r
egion by Linden et al. (1993a) is applicable for at least one order of
magnitude in radius from the Galactic Center (10 ... 100 pc). The vis
cosity nu is shown to be weakly dependent on the radius s: nu approxim
ately s0.4 . Finally, we discuss the influence of the inner boundary o
n the structure of the inner disk regions.