Realistic Magnetohydrodynamical Simulations of Local Solar Supergranulation

Details Realistic Magnetohydrodynamical Simulations of Local Solar Supergranulation Realistic Magnetohydrodynamical Simulations of Local Solar Supergranulation

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..416..427u&link_type=abstract

Solar-Stellar Dynamos as Revealed by Helio- and Asteroseismology: GONG 2008/SOHO 21 ASP Conference Series, Vol. 416, proceedings

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Three-dimensional numerical simulations of solar surface magnetoconvection using realistic model physics are conducted. The thermal structure of convective motions into the upper radiative layers of the photosphere, the main scales of convective cells and the penetration depths of convection are investigated. We take a part of the solar photosphere with horizontal size 60 × 60 Mm by depth 20 Mm from the level of the visible solar surface. We use a realistic initial model of the Sun and apply the equation of state with the opacities of stellar matter. The equations of fully compressible radiative magnetohydrodynamics with dynamical viscosity and gravity are solved. We apply 1) a conservative TVD difference scheme for the magnetohydrodynamics, 2) the diffusion approximation for radiative transfer, and 3) dynamical viscosity from subgrid-scale modeling. In the simulations, we take a uniform two-dimensional grid in the horizontal plane and a nonuniform grid in depth with 600 × 600 × 204 pixels. We use 512 processors with distributed-memory multiprocessors on supercomputer MVS-100k in the Joint Computational Center of the Russian Academy of Sciences.

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