Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout
Abstract
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⊙ zero-metallicity progenitor starting from both 2D and 3D CHIMERA models and a 10 M⊙ 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 56Ni velocities of ~1950 and ~1750 km s-1 at shock breakout from 2D and 3D 9.6 M⊙ 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⊙ model, which achieves maximum 56Ni velocities of ~2500 km s-1 at shock breakout.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- November 2021
- DOI:
- 10.3847/1538-4357/ac1d49
- arXiv:
- arXiv:2106.01389
- Bibcode:
- 2021ApJ...921..113S
- Keywords:
-
- Hydrodynamics;
- Massive stars;
- Core-collapse supernovae;
- Supernovae;
- Stellar evolution;
- 1963;
- 732;
- 304;
- 1668;
- 1599;
- Astrophysics - High Energy Astrophysical Phenomena
- E-Print:
- 31 pages, 23 figures, published in ApJ