  In the first paper of this series, using analytic tools, we examined how the
evolution and structure of a massive accretion disk may be influenced by the
deposition of mass and angular momentum by an infalling Bondi-Hoyle wind. Such
a mass influx impacts the long-term behavior of the disk by providing
additional sources of viscosity and heating. Here, we make improvements over
this earlier work by incorporating the results of 3D hydrodynamical simulations
of the large scale accretion from an ambient medium into the disk evolution
equations developed previously. We discuss two models, one with the axis of the
disk parallel to, and the second with the axis oriented perpendicular to the
large scale Bondi-Hoyle flow. We find that the mass inflow rate onto the disk
within logarithmic annuli is roughly constant with radius and that the
impacting wind carries much less specific angular momentum than Keplerian. We
also find, in general, that the infrared spectrum of a wind-fed disk system is
steeper than that of a Shakura-Sunyaev configuration, due mainly to the
dissipation of the wind's kinetic energy at the disk's surface. In applying our
results to the Galactic Center black hole candidate, Sgr A*, we demonstrate
that a high wind inflow rate of order 10^-4 solar masses per year cannot be
incorporated into a fossil disk without a significant dissipation of kinetic
energy at all radii. Such a high dissipation would violate current infrared and
near-infrared limits on the observed spectrum of Sgr A*.
