1 Theory and Simulations of Solar Atmosphere Dynamics

Abstract

Numerical simulations are used to study the generation and propagation of waves in the solar atmosphere. Solar p-mode oscillations are excited by turbulent pressure work and entropy fluctuations (non-adiabatic gas pressure work) near the solar surface. Interactions between short and long period waves and radiative energy transfer control the formation of shocks. The magnetic structure of the atmosphere induces coupling among various MHD wave modes, with intense coupling and wave transformation at the beta equal one surface, which likely is the location of the so-called “magnetic canopy”.

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@inproceedings{Stein1TA, title={1 Theory and Simulations of Solar Atmosphere Dynamics}, author={R. F. Stein and Tom J. Bogdan and Mats Carlsson and V H Hansteen and A. D. McMurry and Colin S. Rosenthal and {\AA}ke Nordlund} }