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Many planets orbit within an AU of their stars, raising questions about theirorigins. Particularly puzzling are the planets found near the silicatesublimation front. We investigate conditions near the front in the protostellardisk around a young intermediate-mass star, using the first global 3-Dradiation non-ideal MHD simulations in this context. We treat the starlightheating; 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 magnetorotationalturbulence around the sublimation front at 0.5 AU. The disk interior to 0.8 AUis turbulent, with velocities exceeding 10% of the sound speed. Beyond 0.8 AUis the dead zone, cooler than 1000 K and with turbulence orders of magnitudeweaker. A local pressure maximum just inside the dead zone concentrates solidparticles, favoring their growth. Over many orbits, a vortex develops at thedead zones inner edge, increasing the disks thickness locally by around 10%. Wesynthetically observe the results using Monte Carlo transfer calculations,finding the sublimation front is near-infrared bright. The models with netvertical magnetic fields develop extended, magnetically-supported atmospheresthat reprocess extra starlight, raising the near-infrared flux 20%.The vortexthrows a nonaxisymmetric shadow on the outer disk. At wavelengths > 2 micron,the flux varies several percent on monthly timescales. The variations are moreregular when the vortex is present. The vortex is directly visible as an arc atultraviolet through near-infrared wavelengths, given sub-AU spatial resolution.

3D Radiation Non-ideal Magnetohydrodynamical Simulations Of The Inner Rim In Protoplanetary Disks