  Detailed modeling of stellar evolution requires a better understanding of the
(magneto-)hydrodynamic processes which mix chemical elements and transport
angular momentum. Understanding these pro- cesses is crucial if we are to
accurately interpret observations of chemical abundance anomalies, surface
rotation measurements and asteroseismic data. Here, we use two-dimensional
hydrodynamic simula- tions of the generation and propagation of internal
gravity waves (IGW) in an intermediate mass star to measure the chemical mixing
induced by these waves. We show that such mixing can generally be treated as a
diffusive process. We then show that the local diffusion coefficient does not
depend on the local fluid velocity, but rather on the wave amplitude. We then
use these findings to provide a simple parametrization for this diffusion which
can be incorporated into stellar evolution codes and tested against
observations.
