  It is thought that many characteristics of the gaseous features within the
central parsec of our Galaxy, are associated with the accretion of ambient
plasma by a central concentration of mass. Using a 3D hydrodynamical code, we
have been simulating this process in order to realistically model the gaseous
flows in the center of our Galaxy. In the most recent simulation, we have taken
into account the multi-point-like distribution of stellar wind sources, as well
as the magnetic heating and radiative cooling of these stellar winds. As
expected, we find that the structure of the flow is significantly different
from that due to a uniform medium. We also investigate the possibility that Sgr
A* is due to a distributed mass concentration instead of the canonical point
mass of a black hole. We discuss the physical state of the accreting gas and
how our results suggest that Sgr A* is unlikely to be associated with a ``dark
cluster''.
