Supercomputing Stars

Formulating a predictive model of stellar evolution requires a robust model of high Reynolds number turbulence, due to a variety of instabilities, under a broad range of conditions. This project is tantamount to extending the classical theories of hydrodynamic turbulence beyond the isotropic, homogeneous, incomprDessible case to situations in which anisotropy, stratiification, and compressibility are essential elements. I will discuss some of the recent progress that has been made in this direction and highlight the role that has been played by large scale hydrodynamic simulation.