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

Published online by Cambridge University Press:  23 January 2015

W. David Arnett
W. David Arnett*
Affiliation:
Steward Observatory, University of Arizona, Tucson AZ 85721, USA email: darnett@as.arizona.edu
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Abstract

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This is a sketch of a 321D approximation which is nonlocal, and thus has nonzero fluxes of KE (to be published in more detail elsewhere). We plan to add this as an option to MESA. Inclusion of KE fluxes seems to help resolve the solar abundance problem (Asplund et al.2009). Smaller cores may ease the explosion problems with core collapse supernova simulations.

Keywords

convectionturbulenceSun: abundancesstars: evolutionsupernovae

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