Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout

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-circle dot zero-metallicity progenitor starting from both 2D and 3D Chimera models and a 10 M-circle dot 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 Ni-56 velocities of similar to 1950 and similar to 1750 km s(-1) at shock breakout from 2D and 3D 9.6 M-circle dot Chimera models, respectively, due to the bullets' ability to penetrate the He/H shell. When mapping from 2D, we find that the development of higher-velocity structures is suppressed when the 2D Chimera model and 3D FLASH model meshes are aligned. The development of faster-growing spherical-bubble structures, as opposed to the slower-growing toroidal structure imposed by axisymmetry, allows for interaction of the bullets with the shock and seeds further R-T instabilities at the He/H interface. We see similar effects in the 10 M-circle dot model, which achieves maximum Ni-56 velocities of similar to 2500 km s(-1) at shock breakout.

Automated summary

The study presents three-dimensional simulations of core-collapse supernovae using the FLASH code, with results indicating the influence of the relative velocity difference between the supernova shock and the metal-rich Rayleigh-Taylor bullets on the final morphology of the explosion.