  In an attempt to understand the properties of convective energy transport in
the solar convection zone, a numerical model has been constructed for turbulent
flows in a compressible, radiation-coupled, non-magnetic, gravitationally
stratified medium using a realistic equation of state and realistic opacities.
The time-dependent, three-dimensional hydrodynamic equations are solved with
minimal simplifications.
  The statistical information obtained from the present simulation provides an
improved understanding of solar photospheric convection. The characteristics of
solar convection in shallow regions is parameterized and compared with the
results of Chan and Sofia's simulations of deep and efficient convection (Chan
and Sofia 1989). We assess the importance of the zones of partial ionization in
the simulation, and confirm that the radiative energy transfer is negligible
throughout the region except in the uppermost scale heights of the convection
zone, a region of very high super-adiabaticity.
  When the effects of partial ionization are included, the dynamics of flows
are altered significantly. However, we confirm the Chan and Sofia result that
kinetic energy flux is non-negligible and can have a negative value in the
convection zone.
