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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...
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Published in: | The Astrophysical journal 2021-11, Vol.921 (2), p.113 |
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Main Authors: | , , , , |
Format: | Article |
Language: | English |
Subjects: | |
Citations: | Items that this one cites Items that cite this one |
Online Access: | Get full text |
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Summary: | 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
56
Ni 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
56
Ni velocities of ∼2500 km s
−1
at shock breakout. |
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ISSN: | 0004-637X 1538-4357 |
DOI: | 10.3847/1538-4357/ac1d49 |