  Results of realistic simulations of solar surface convection on the scale of
supergranules (96 Mm wide by 20 Mm deep) are presented. The simulations cover
only 10% of the geometric depth of the solar convection zone, but half its
pressure scale heights. They include the hydrogen, first and most of the second
helium ionization zones. The horizontal velocity spectrum is a power law and
the horizontal size of the dominant convective cells increases with increasing
depth. Convection is driven by buoyancy work which is largest close to the
surface, but significant over the entire domain. Close to the surface buoyancy
driving is balanced by the divergence of the kinetic energy flux, but deeper
down it is balanced by dissipation. The damping length of the turbulent kinetic
energy is 4 pressure scale heights. The mass mixing length is 1.8 scale
heights. Two thirds of the area is upflowing fluid except very close to the
surface. The internal (ionization) energy flux is the largest contributor to
the convective flux for temperatures less than 40,000 K and the thermal energy
flux is the largest contributor at higher temperatures. This data set is useful
for validating local helioseismic inversion methods. Sixteen hours of data are
available as four hour averages, with two hour cadence, at
steinr.msu.edu/~bob/96averages, as idl save files. The variables stored are the
density, temperature, sound speed, and three velocity components. In addition,
the three velocity components at 200 km above mean continuum optical depth
unity are available at 30 sec. cadence.
