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Hydrodynamics of nuclear combustion for stars from the early Universe

Stellar evolution at very low and zero metallicity features convective mixing of proton-rich material into convective 12C-rich He-burning regions. During such events nuclear and convective mixing time scales are similar and substantial nuclear energy release into the hydrodynamic flow implies a combustion regime that can not be described with spherically symmetric stellar evolution assumptions. I will report on 3D stellar hydrodynamics simulations of stellar combustion, including their verification and validation. The implications of our simulation results for the origin of the elements in the first generations of stars and galactic chemical evolution will be presented.

Cody Hall

Falk Herwig (U of Victoria)

November 23, 2012
14:00 - 15:00