Simulation of Solar Magneto-Convection
We describe the methods for realistic three-dimensional, time-dependent simulations of the interaction between convective flows, magnetic field and radiation near the visible solar surface and show some results recent of our computations: 1) the formation of magnetic patterns and small-scale intense magnetic fields for different amount of magnetic flux in the computational domain and, 2) the structure and dynamics of a larger flux concentration, a so-called pore. Experiences with running our code on the Hitachi SR80000 of HLRB are briefly described.
KeywordsConvection Zone Colour Version Radiative Transfer Equation Solar Photosphere Convective Energy Transport
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