  We demonstrate that our Galactic Center, despite little evidence for the
presence of a currently active nucleus, provides insight into the feeding of
AGN: The observed velocity field of molecular clouds can be interpreted as
tracing out the spiralling inwards of gas in a large accretion flow towards the
Galactic Center (Linden et al. 1993, Biermann et al. 1993) in the radial
distance range from a few parsec to a few hundred pc. The required effective
viscosity corresponds well to the observed turbulent velocities and
characteristic length scales. The implied mass influx provides indeed all the
material needed to maintain the presently observed star formation rate at
distances closer than about $100$ pc. We argue that the energy input from
supernova explosions due to the high rate of star formation can feed the
turbulence of the interstellar medium. This then keeps the effective viscosity
high as required to feed the star formation. We suggest that this process leads
to limit cycles in star formation, and as a consequence also to limit cycles in
the feeding of any activity at the very center.
