  Three-dimensional magnetohydrodynamical large eddy simulations of solar
surface convection 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
is investigated. We simulate a some portion of the solar photosphere and the
upper layers of the convection zone, a region extending 30 x 30 Mm horizontally
from 0 Mm down to 18 Mm below the visible surface. We solve equations of the
fully compressible radiation magnetohydrodynamics with dynamical viscosity and
gravity. For numerical simulation we use: 1)realistic initial model of Sun and
equation of state and opacities of stellar matter, 2) high order conservative
TVD scheme for solution magnetohydrodynamics, 3) diffusion approximation for
solution radiative transfer 4) calculation dynamical viscosity from 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 supercomputer MBC-1500 with distributed memory multiprocessors in Russian
Academy of Sciences.
