Turbulent Mixing in Stars: Theoretical Hurdles
arXiv:0912.2978 · doi:10.1017/S174392131000030X
Abstract
A program is outlined, and first results described, in which fully three-dimensional, time dependent simulations of hydrodynamic turbulence are used as a basis for theoretical investigation of the physics of turbulence in stars. The inadequacy of the treatment of turbulent convection as a diffusive process is discussed. A generalization to rotation and magnetohydrodynamics is indicated, as are connection to simulations of 3D stellar atmospheres.
5 pages, 1 figure, IAU Symposium 265, 2009