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

**Authors:** Michael A. Sandoval, W. Raphael Hix, O. E. Bronson Messer, Eric J. Lentz, J. Austin Harris  
**arXiv:** [2106.01389](https://arxiv.org/abs/2106.01389)  
**Date:** 2021-06-02  
**Summary page:** https://www.summarizepaper.com/en/paper/2106.01389v2/

## Key points

- Sandoval et al. present cutting-edge three-dimensional simulations of core-collapse supernovae using the FLASH code
- The study focuses on two distinct progenitor scenarios: a 9.6-$M_{\odot}$ zero-metallicity star and a 10-$M_{\odot}$ solar-metallicity progenitor
- Monitoring of 160 nuclear species throughout simulations until shock breakout in 3D reveals the crucial role of relative velocity difference between supernova shock and metal-rich Rayleigh-Taylor "bullets"
- Maximum $^{56}\rm{Ni}$ velocities reaching approximately $1950~\rm{km~s}^{-1}$ and $1750~\rm{km~s}^{-1}$ observed at shock breakout from 2D and 3D 9.6-$M_{\odot}$ CHIMERA models respectively
- Transitioning from 2D to corresponding 3D models shows suppressed development of higher velocity structures when mesh alignments are maintained, leading to emergence of faster-growing spherical-bubble structures facilitating interactions between bullets and shocks
- Remarkable maximum $^{56}\rm{Ni}$ velocities around $2500~\rm{km~s}^{-1}$ achieved at shock breakout in investigation involving a 10-$M_{\odot}$ model
- Findings highlight intricate interplays between shock dynamics, metal-rich ejecta behavior, and morphological evolution influencing core-collapse supernova outcomes

## Summary

In their study, Sandoval et al. present cutting-edge three-dimensional simulations of core-collapse supernovae using the FLASH code. These simulations meticulously track the evolution of the explosion from its inception to the stellar surface. The team focuses on two distinct progenitor scenarios: a 9.6-$M_{\odot}$ zero-metallicity star initiated from both 2D and 3D CHIMERA models, and a 10-$M_{\odot}$ solar-metallicity progenitor stemming from a 2D CHIMERA model. Throughout their simulations, which extend until shock breakout in 3D, they meticulously monitor the behavior of 160 nuclear species. A key finding of their research is the crucial role played by the relative velocity difference between the supernova shock and metal-rich Rayleigh-Taylor (R-T) "bullets" in shaping the evolution of metal-rich ejecta as it traverses through the density profile of the progenitor star. This velocity differential ultimately dictates the final morphology of the explosion. Notably, maximum $^{56}\rm{Ni}$ velocities reaching approximately $1950~\rm{km~s}^{-1}$ and $1750~\rm{km~s}^{-1}$ are observed at shock breakout from 2D and 3D 9.6-$M_{\odot}$ CHIMERA models respectively due to bullets' ability to penetrate through the He/H shell. Transitioning from 2D models to their corresponding 3D counterparts reveals intriguing phenomena such as suppressed development of higher velocity structures when mesh alignments are maintained between 2D CHIMERA and 3D FLASH models. The emergence of faster-growing spherical-bubble structures in lieu of slower-growing toroidal formations enforced by axisymmetry facilitates interactions between bullets and shocks, seeding additional R-T instabilities at critical interfaces like He/H boundaries. The team also notes analogous effects in their investigation involving a 10-$M_{\odot}$ model, where they achieve remarkable maximum $^{56}\rm{Ni}$ velocities around $2500~\rm{km~s}^{-1}$ at shock breakout. These findings collectively underscore how intricate interplays between shock dynamics, metal-rich ejecta behavior, and morphological evolution significantly influence core-collapse supernova outcomes. Ultimately, this comprehensive study sheds new light on key mechanisms governing these cataclysmic cosmic events and provides valuable insights into understanding their complex nature.