  The radio source Sagittarius A* (Sgr A*) is believed to be a hot,
inhomogeneous, magnetized plasma flowing near the event horizon of the 3
million solar mass black hole at the galactic center. At a distance of 8000
parsecs the black hole would be among the largest black holes as judged by
angular size. Recent observations are consistent with the idea that the
millimeter and sub-millimeter photons are dominated by optically thin, thermal
synchrotron emission. Anticipating future Very Long Baseline Interferometry
(VLBI) observations of Sgr A* at these wavelengths, we present here the first
dynamically self-consistent models of millimeter and sub-millimeter emission
from Sgr A* based on general relativistic numerical simulations of the
accretion flow. Angle-dependent spectra are calculated assuming a thermal
distribution of electrons at the baryonic temperature dictated by the
simulation and the accretion rate, which acts as a free parameter in our model.
The effects of varying model parameters (black hole spin and inclination of the
spin to the line of sight) and source variability on the spectrum are shown. We
find that the accretion rate value needed to match our calculated millimeter
flux to the observed flux is consistent with constraints on the accretion rate
inferred from detections of the rotation measure. We also describe the
relativistic jet that is launched along the black hole spin axis by the
accretion disk and evolves to scales of 1000 gravitational radii.
