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Title: 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 seedsmore » 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.« less

Authors:
ORCiD logo [1]; ORCiD logo [2]; ORCiD logo [2]; ORCiD logo [1]; ORCiD logo [3]
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  1. Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
  2. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Univ. of Tennessee, Knoxville, TN (United States)
  3. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
Sponsoring Org.:
USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF); USDOE National Nuclear Security Administration (NNSA)
OSTI Identifier:
1831662
Grant/Contract Number:  
AC05-00OR22725; PHY-1516197; PHY-1913531
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal
Additional Journal Information:
Journal Volume: 921; Journal Issue: 2; Journal ID: ISSN 0004-637X
Publisher:
IOP Publishing
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Hydrodynamics; Massive stars; Core-collapse supernovae; Supernovae; Stellar evolution

Citation Formats

Sandoval, Michael A., Hix, W. Raphael, Messer, O. Bronson, Lentz, Eric J., and Harris, J. Austin. Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout. United States: N. p., 2021. Web. doi:10.3847/1538-4357/ac1d49.
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Sandoval, Michael A., Hix, W. Raphael, Messer, O. Bronson, Lentz, Eric J., & Harris, J. Austin. Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout. United States. https://doi.org/10.3847/1538-4357/ac1d49
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Sandoval, Michael A., Hix, W. Raphael, Messer, O. Bronson, Lentz, Eric J., and Harris, J. Austin. Mon . "Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout". United States. https://doi.org/10.3847/1538-4357/ac1d49. https://www.osti.gov/servlets/purl/1831662.
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@article{osti_1831662,
title = {Three-dimensional Core-collapse Supernova Simulations with 160 Isotopic Species Evolved to Shock Breakout},
author = {Sandoval, Michael A. and Hix, W. Raphael and Messer, O. Bronson and Lentz, Eric J. and Harris, J. Austin},
abstractNote = {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.},
doi = {10.3847/1538-4357/ac1d49},
journal = {The Astrophysical Journal},
number = 2,
volume = 921,
place = {United States},
year = {2021},
month = {11}
}
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