Radiation Transfer of Models of Massive Star Formation. II. Effects of
  the Outflow
  (Abridged) We present radiation transfer simulations of a massive (8 Msun)
protostar forming from a massive (Mc=60 Msun) protostellar core, extending the
model developed by Zhang & Tan (2011). The two principal improvements are (1)
developing a model for the density and velocity structure of a disk wind that
fills the bipolar outflow cavities; and (2) solving for the radially varying
accretion rate in the disk due to a supply of mass and angular momentum from
the infall envelope and their loss to the disk wind. One consequence of the
launching of the disk wind is a reduction in the amount of accretion power that
is radiated by the disk. For the transition from dusty to dust-free conditions
where gas opacities dominate, we now implement a gradual change as a more
realistic approximation of dust destruction. We study how the above effects,
especially the outflow, influence the SEDs and the images of the protostar.
Dust in the outflow cavity significantly affects the SEDs at most viewing
angles. It further attenuates the short-wavelength flux from the protostar,
controlling how the accretion disk may be viewed, and contributes a significant
part of the near- and mid-IR fluxes. These fluxes warm the disk, boosting the
mid- and far-IR emission. We find that for near face-on views, the SED from the
near-IR to about 60 micron is very flat, which may be used to identify such
systems. We show that the near-facing outflow cavity and its walls are still
the most significant features in images up to 70 micron, dominating the mid-IR
emission and determining its morphology. The thermal emission from the dusty
outflow itself dominates the flux at ~20 micron. The detailed distribution of
the dust in the outflow affects the morphology, for example, even though the
outflow cavity is wide, at 10 to 20 micron, the dust in the disk wind can make
the outflow appear narrower than in the near-IR bands.
