Radiation Transfer of Models of Massive Star Formation. III. The
  Evolutionary Sequence
  We present radiation transfer (RT) simulations of evolutionary sequences of
massive protostars forming from massive dense cores in environments of high
surface densities. The protostellar evolution is calculated with a detailed
multi-zone model, with the accretion rate regulated by feedback from an
evolving disk-wind outflow cavity. Disk and envelope evolutions are calculated
self-consistently. In this framework, an evolutionary track is determined by
three environmental initial conditions: the initial core mass M_c, the mean
surface density of the ambient star-forming clump Sigma_cl, and the
rotational-to-gravitational energy ratio of the initial core, beta_c.
Evolutionary sequences with various M_c, Sigma_cl, beta_c are constructed. We
find that in a fiducial model with M_c=60Msun, Sigma_cl=1 g/cm^2 and
beta_c=0.02, the final star formation efficiency >~0.43. For each evolutionary
track, RT simulations are performed at selected stages, with temperature
profiles, SEDs, and images produced. At a given stage the envelope temperature
is highly dependent on Sigma_cl, but only weakly dependent on M_c. The SED and
MIR images depend sensitively on the evolving outflow cavity, which gradually
wides as the protostar grows. The fluxes at <~100 microns increase
dramatically, and the far-IR peaks move to shorter wavelengths. We find that,
despite scatter caused by different M_c, Sigma_cl, beta, and inclinations,
sources at a given evolutionary stage appear in similar regions on color-color
diagrams, especially when using colors at >~ 70 microns, where the scatter due
to the inclination is minimized, implying that such diagrams can be useful
diagnostic tools of evolutionary stages of massive protostars. We discuss how
intensity profiles along or perpendicular to the outflow axis are affected by
environmental conditions and source evolution.
