  The dynamics and thermal structure of the surface layers of stars with outer
convection zones can be studied in some detail by means of numerical
simulations of time-dependent compressible convection. In an effort to
investigate the properties of ``stellar granulation'' as a function of spectral
type, we have carried out elaborate 2-dimensional radiation hydrodynamics
calculations of surface convection for a variety of stellar parameters. The
main features of these simulations are reviewed, with particular reference to
standard mixing length models.
