  We present numerical simulations of penetrative convection and gravity wave
excitation in the Sun. Gravity waves are self-consistently generated by a
convective zone overlying a radiative interior. We produce power spectra for
gravity waves in the radiative region as well as estimates for the energy flux
of gravity waves below the convection zone. We calculate a peak energy flux in
waves below the convection zone to be three orders of magnitude smaller than
previous estimates for m=1. The simulations show that the linear dispersion
relation is a good approximation only deep below the convective-radiative
boundary. Both low frequency propagating gravity waves as well as higher
frequency standing modes are generated; although we find that convection does
not continually drive the standing g-mode frequencies.
