  I represent results three-dimensional numerical simulation of solar surface
convection on scales local supergranulation with realistic model physics. I
study thermal structure of convective motions in photosphere, the range of
convection cell sizes and the penetration depths of convection. A portion of
the solar photosphere extending 100 x 100 Mm horizontally and from 0 Mm down to
20 Mm below the visible surface is considered. I take equation of state and
opacities of stellar matter and distribution with radius of all physical
variables from Solar Standard Model. The equations of fully compressible
radiation hydrodynamics with dynamical viscosity and gravity are solved. The
high order conservative PPML difference scheme for the hydrodynamics, the
method of characteristic for the radiative transfer and dynamical viscosity
from subgrid scale modeling are applied. The simulations are conducted on a
uniform horizontal grid of 1000 x 1000, with 168 nonuniformly spaced vertical
grid points, on 256 processors with distributed memory multiprocessors on
supercomputer MVS5000 in Computational Centre of Russian Academy of Sciences.
