Speaker
Description
Predicting the outcome of core collapse in massive stars (whether the star explodes as a supernova or collapses into a black hole) remains an open problem. The complex physics involved and the uncertainties in progenitor structure make it difficult to identify which stars are more likely to explode. Recent studies suggest that the density gradient at the interface between the silicon and oxygen shells may play an important role in determining the explosion outcome. To investigate this effect, we perform simulations of synthetic progenitors in which the density contrast at this interface is systematically varied while all other parameters are kept fixed. The simulations are carried out in two dimensions, including general relativistic gravity and M1 neutrino transport.
