  We present numerical simulations of internal gravity waves (IGW) in a star
with a convective core and extended radiative envelope. We report on
amplitudes, spectra, dissipation and consequent angular momentum transport by
such waves. We find that these waves are generated efficiently and transport
angular momentum on short timescales over large distances. We show that, as in
the Earth's atmosphere, IGW drive equatorial flows which change magnitude and
direction on short timescales. These results have profound consequences for the
observational inferences of massive stars, as well as their long term angular
momentum evolution. We suggest IGW angular momentum transport may explain many
observational mysteries, such as: the misalignment of hot Jupiters around hot
stars, the Be class of stars, Ni enrichment anomalies in massive stars and the
non-synchronous orbits of interacting binaries.
