  We present hydrodynamic simulations of the inner few parsecs of the Milky
Way's Galactic Center that, for the first time, combine a realistic treatment
of stellar winds and the circumnuclear disk as they interact with the
gravitational potential of the nuclear star cluster and Sagittarius~A*. We
observe a complex interaction of the stellar winds with the inner edge of the
circumnuclear disk, which leads to the growth of instabilities, induced
accretion of cool gas from the inner edge of the disk, and the eventual
formation of a small accretion disk of $\sim 10^4-10^5$ K within $r \sim 0.1$
pc.
