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The incorporation of realistic microphysics with modern hydrodynamical methods gives new opportunities to solve recalcitrant problems of stellar evolution, especially those involving rapid change. Examples to illustrate such progress will include (1) convective oxygen burning in massive stars, (2) flames and detonations in Type~I supernovae, (3) Novae, (4) Accretion, (5) Instabilities driving mixing, and (6) Explosive nucleosynthesis and the mass cut in Type~II supernovae. Future prospects for improvement from hardware, algorithms, and better understanding will be discussed.
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