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Convection in Stars Proceedings IAU Symposium No. 239, 2007

Summary: Convection in Stars
Proceedings IAU Symposium No. 239, 2007
F. Kupka , I.W. Roxburgh & K. L. Chan, eds.
# 2007 International Astronomical Union
DOI: 00.0000/X000000000000000X
Stellar Convection with Nuclear Burning
David Arnett,
Casey Meakin, and Patrick A. Young
Steward Observatory, University of Arizona, Tucson AZ 85721, USA
email: darnett@as.arizona.edu
Abstract. Careful choice of of method, problem, and zoning has allowed us to do three­
dimensional (3D) simulations of thermally relaxed, nearly adiabatic convection (with nuclear
burning). The simulations are run long enough so that a robust statistical state is found. We
find that 2D simulations are biased relative to 3D simulations: 2D shows larger velocities and
less mixing than their 3D counterparts. Detailed theoretical analysis of these numerical exper­
iments allows us to begin to build a simple theoretical model of turbulent convection in stars,
which may be used in 1D calculations of stellar evolution. Implications for stellar evolution, will
be discussed. Oxygen shell burning simulations in 3D, and multishell burning of C, Ne, O, and
Si in 2D will be presented, as will aspherical distortion in supernovae progenitors (Meakin and


Source: Arnett, W. David - Department of Astronomy, University of Arizona


Collections: Physics