  Many planets orbit within an AU of their stars, raising questions about their
origins. Particularly puzzling are the planets found near the silicate
sublimation front. We investigate conditions near the front in the protostellar
disk around a young intermediate-mass star, using the first global 3-D
radiation non-ideal MHD simulations in this context. We treat the starlight
heating; the silicate grains sublimation and deposition at the local,
time-varying temperature and density; temperature-dependent Ohmic dissipation;
and various initial magnetic fields. The results show magnetorotational
turbulence around the sublimation front at 0.5 AU. The disk interior to 0.8 AU
is turbulent, with velocities exceeding 10% of the sound speed. Beyond 0.8 AU
is the dead zone, cooler than 1000 K and with turbulence orders of magnitude
weaker. A local pressure maximum just inside the dead zone concentrates solid
particles, favoring their growth. Over many orbits, a vortex develops at the
dead zones inner edge, increasing the disks thickness locally by around 10%. We
synthetically observe the results using Monte Carlo transfer calculations,
finding the sublimation front is near-infrared bright. The models with net
vertical magnetic fields develop extended, magnetically-supported atmospheres
that reprocess extra starlight, raising the near-infrared flux 20%.The vortex
throws a nonaxisymmetric shadow on the outer disk. At wavelengths > 2 micron,
the flux varies several percent on monthly timescales. The variations are more
regular when the vortex is present. The vortex is directly visible as an arc at
ultraviolet through near-infrared wavelengths, given sub-AU spatial resolution.
