Magnetohydrodynamic Processes in the Surface Layers of the Sun

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Project Summary Lou/ATM-9320357 This project will focus on magnetohydrodynamic physical processes likely to be involved in solar chromospheric and coronal activity. The research is a continuation of past efforts to understand the mechanisms by which waves generated in the convective zones of stars propagate into the magnetized outer atmospheric layers, and the physical effects arising from this wave propagation. Specific goals of this continuation are: (1) to model the extended heating of the inner solar wind via resonant absorption of Alfven waves; (2) to construct analytical models for the reflection and transmission of Alfven waves in inhomogeneous atmospheres, all outside the WKB approximation; and (3) to develop numerical experiments for the simulation of both resonant absorption and reflection of Alfven waves, and compare results from these experiments to the analytical results.