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Paper: Three Dimensional Numerical Simulation of MHD Solar Convection on Multiprocessors Supercomputer Systems
Volume: 354, Solar MHD Theory and Observations: A High Spatial Resolution Perspective
Page: 115
Authors: Ustyugov, S.D.
Abstract: Three-dimensional magnetohydrodynamical large eddy simulations of solar surface convection using realistic model physics are conducted. The effects of magnetic fields on the thermal structure of convective motions into radiative layers, the range of convection cell sizes and the penetration depths of convection are investigated. We simulate a portion of the solar photosphere and the upper layers of the convection zone, a region extending 18 × 18 Mm horizontally from 0 Mm down to 18 Mm below the visible surface. We solve the equations of fully compressible radiation magnetohydrodynamics with dynamical viscosity and gravity. We use: 1) a high order conservative TVD scheme for the magnetohydrodynamics, 2) the diffusion approximation for the radiative transfer, 3) dynamical viscosity from subgrid scale modeling. We start from a realistic initial model of Sun with an equation of state and opacities of stellar matter. The simulations are conducted on a uniform horizontal grid of 192 192, with 144 nonuniformly spaced vertical grid points, on 64 processors with distributed memory multiprocessors.
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