Realistic solar convection simulations

We report on realistic simulations of solar surface convection that are ess entially parameter-free, but include detailed physics in the equation of st ate and radiative energy exchange. The simulation results are compared quan titatively with observations. Excellent agreement is obtained for the distr ibution of the emergent continuum intensity, the profiles of weak photosphe ric lines, the p-mode frequencies, the asymmetrical shape of the mode veloc ity and intensity spectra, the p-mode excitation rate, and the depth of the convection zone. We describe how solar convection is non-local. It is driv en from a thin surface thermal boundary layer where radiative cooling produ ces low entropy gas which forms the cores of the downdrafts in which most o f the buoyancy work occurs. Turbulence and vorticity are mostly confined to the intergranular lanes and underlying downdrafts. Finally, we present som e preliminary results on magneto-convection.