HR: 1340h
AN: SH23A-1167    [Abstracts]
TI: Realistic Numerical Simulations of Solar Magneto-Convection and Oscillations
AU: * Jacoutot, L
EM: jacoutot@stanford.edu
AF: Center for Turbulence Research, Bldg 500 480 Escondido Mall, Stanford, CA 94305, United States
AU: Kosovichev, A G
EM: sasha@quake.Stanford.EDU
AF: Hansen Experimental Physics Laboratory, 452 Lomita Mall, Stanford, CA 94305, United States
AU: Mansour, N N
EM: nmansour@mail.arc.nasa.gov
AF: NASA Ames Research Center, 801 Moffett Blvd, Mountain View, CA 94043, United States
AU: Wray, A
EM: wray@nas.nasa.gov
AF: NASA Ames Research Center, 801 Moffett Blvd, Mountain View, CA 94043, United States
AB: 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.
DE: 7524 Magnetic fields
DE: 7529 Photosphere
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting