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We introduce two new methods that are designed to improve the realism andutility of large, active region-scale 3D MHD models of the solar atmosphere. Weapply these methods to RADMHD, a code capable of modeling the Sun's upperconvection zone, photosphere, chromosphere, transition region, and coronawithin a single computational volume. We first present a way to approximate thephysics of optically-thick radiative transfer without having to take thecomputationally expensive step of solving the radiative transfer equation indetail. We then briefly describe a rudimentary assimilative technique thatallows a time series of vector magnetograms to be directly incorporated intothe MHD system.

Improving Large-scale Convection Zone-to-Corona Models