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R. G. Deupree (Los Alamos National Laboratory)
2D stellar evolution sequences including rotation are calculated into core helium burning. These reveal that the convection zone that forms above the burning region near the beginning of hydrogen shell burning is larger at the equator than at the pole for at least rapidly rotating models. Fully implicit, 2d hydrodynamic simulations of selected models show that this asymmetry is maintained. Such hydrodynamic simulations for both nonrotating and rotating models also show that the overshooting beyond the top of this convective shell is a few tenths of a pressure scale height, but that the overshooting out the bottom of the convective shell is very small. This work is supported by NASA ATP grant S-92660-F and by the US Department of Energy.
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.