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Turbulent Mixing in Stars: Theoretical Hurdles

Published online by Cambridge University Press:  09 March 2010

W. David Arnett  and
Casey Meakin
W. David Arnett
Affiliation:
Steward Observatory, University of Arizona, 933 Cherry Avenue, Tucson, Arizona 85721, USA email: darnett@as.arizona.edu, casey.meakin@gmail.com
Casey Meakin
Affiliation:
Steward Observatory, University of Arizona, 933 Cherry Avenue, Tucson, Arizona 85721, USA email: darnett@as.arizona.edu, casey.meakin@gmail.com
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Abstract

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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. The inadequacy of the treatment of turbulent convection as a diffusive process is indicated. A generalization to rotation and magnetohydrodynamics is indicated, as are connections to simulations of 3D stellar atmospheres.

Keywords

turbulenceconvectionhydrodynamicsrotationwavesnucleosynthesisplasmastars: supernovaestars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 106 - 110
Copyright
Copyright © International Astronomical Union 2010

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