3D and Some Other Things Missing from the Theory of Massive Star Evolution

摘要: This is a sketch of 321D approximation for stellar convection which nonlocal, and thus has nonzero fluxes KE (to be published in more detail elsewhere). Boundary conditions are discussed fluid dynamics context (i.e., predictions overshoot, semiconvection entrainment analyzed). We plan to add this as an option MESA. Inclusion seems help resolve the solar abundance problem (Asplund 2009). Smaller cores may ease explosion problems with core collapse supernova simulations.