Realistic Numerical Simulations of Solar Magneto-Convection and Oscillations

Details Realistic Numerical Simulations of Solar Magneto-Convection and Oscillations Realistic Numerical Simulations of Solar Magneto-Convection and Oscillations

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh23a1167j&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH23A-1167

Physics

7524 Magnetic Fields, 7529 Photosphere

Scientific paper

The objective of this research is to study how magnetic field affects the structure and dynamics of solar convection and the sources that drive the waves in the Sun. We use a 3D, compressible, non-linear radiative magnetohydrodynamics code developed by Dr. A. Wray for simulating the upper solar photosphere and lower atmosphere. This code takes into account several physical phenomena: compressible fluid flow in a highly stratified medium, radiative energy transfer between the fluid elements, magnetic phenomena, and a real-gas equation of state. Magnetic fields play a crucial role in the structure and heating of the outer atmosphere. Our objectives are to understand the processes related to magnetic fields in this zone. We investigate the interaction between convection, magnetic fields, and oscillations.

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