Numerical simulation of solar magnetoconvection with realistic physics

Three-dimensional magnetohydrodynamics numerical simulation of solar surface convection on scale of supergranulation using realistic model physics is conducted. The effects of magnetic fields on thermal structure of convective motions into radiative layers, the range of convection cell sizes and penetration depths of convection are investigated. We simulate a part of the solar photosphere and the upper layers of the convection zone, a region extending on 30 x 30 Mm horizontally from 0 Mm down to 18 Mm below the visible surface. Equations of the compressible radiation magnetchydrodynamics with dynamical viscosity and gravity are solved. We used: 1) distribution by radius of all variables from realistic model of Sun, 2) equation of state and opacities of matter for stellar conditions, 3) high order conservative TVD scheme for solution of the magnetohydrodynamics equations, 4) diffusion approximation for radiative transfer solution, 5) calculation dynamical viscosity applying subgrid scale modelling. Simulations are conducted on horizontal uniform grid of 320 x 320 and with 144 nonuniformly spaced vertical grid points on the 128 processors of super-computer with distributed memory multiprocessors in Russian Academy of Sciences in Moscow.