A training and research plan is described for the continued development and application of an already existing two- dimensional radiation magnetohydrodynamics (MHD) code to problems in astrophysics. Applications will be performed for three important problems: accretion disk dynamics, molecular cloud collapse during star formation, and the dynamics of the solar corona. Planned improvements to the treatment of the microphysics in the code is expected to produce more realistic results. Utilizing the already implemented algorithm for solving the radiation transfer equation in two-dimensions, self- consistent radiation intensity maps will be computed during the course of these simulations for direct comparison with observations, forming the basis of an interactive "numerical observatory". The code will be implemented on a variety of machines at the NCSA to benchmark the performance of different architectures on the algorithms for MHD and radiation transfer. IN particular, the code will be implemented on the massively parallel Connection Machine.
