Three Dimensional Core-Collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout

Understand

We present three-dimensional simulations of core-collapse supernovae using the FLASH code that follow the progression of the explosion to the stellar surface, starting from neutrino-radiation hydrodynamic simulations of the neutrino-driven phase performed with the CHIMERA code.

• We consider a 9.6-$M_{\odot}$ zero-metallicity progenitor starting from both 2D and 3D CHIMERA models, and a 10-$M_{\odot}$ solar-metallicity progenitor starting from a 2D CHIMERA model, all simulated until shock breakout in 3D while tracking 160 nuclear species.
• The relative velocity difference between the supernova shock and the metal-rich Rayleigh-Taylor (R-T) "bullets" determines how the metal-rich ejecta evolves as it propagates through the density profile of the progenitor and dictates the final morphology of the explosion.
• We find maximum $^{56}\rm{Ni}$ velocities of ${\sim} 1950~\rm{km~s}^{-1}$ and ${\sim} 1750~\rm{km~s}^{-1}$ at shock breakout from 2D and 3D 9.6-$M_{\odot}$ CHIMERA models, respectively, due to the bullets' ability to penetrate the He/H shell.