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Title: Revival of the fittest: exploding core-collapse supernovae from 12 to 25 M⊙

Abstract

Here, we present results of 2D axisymmetric core-collapse supernova simulations, employing the FORNAX code, of nine progenitor models spanning 12 to 25 M⊙. Four of the models explode with inelastic scattering off electrons and neutrons as well as the many-body correction to neutrino-nucleon scattering opacities. We show that these four models feature sharp Si–O interfaces in their density profiles, and that the corresponding dip in density reduces the accretion rate around the stalled shock and prompts explosion. The non-exploding models lack such a steep feature, highlighting the Si–O interface as one key to explosion. Furthermore, we show that all of the non-exploding models can be nudged to explosion with modest changes to macrophysical inputs, including moderate rotation and perturbations to infall velocities, as well as to microphysical inputs, including reasonable changes to neutrino-nucleon interaction rates, suggesting that all the models are perhaps close to criticality. Exploding models have energies of a few × 10 50 erg at the end of our simulation, and are rising, emphasizing the need to continue these simulations over larger grids and for longer times to reproduce the energies seen in nature. Morphology of the explosion contributes to the explosion energy, with more isotropic ejecta producingmore » larger explosion energies. We do not find evidence for the Lepton-number Emission Self-sustained Asymmetry. Finally, we look at proto-neutron star (PNS) properties and explore the role of dimension in our simulations. We find that convection in the PNS produces larger PNS radii as well as greater ‘ν μ’ luminosities in 2D compared to 1D.« less

Authors:
ORCiD logo [1];  [1];  [2];  [3]; ORCiD logo [4]
  1. Princeton Univ., NJ (United States). Dept. of Astrophysical Sciences
  2. Inst. for Advanced Study, Princeton, NJ (United States); Princeton Univ., NJ (United States). Dept. of Astrophysical Sciences
  3. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  4. Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); National Science Foundation (NSF)
OSTI Identifier:
1441344
Report Number(s):
LA-UR-18-20409
Journal ID: ISSN 0035-8711
Grant/Contract Number:
AC52-06NA25396; PHY-1523261; AST-1714267; NSF PHY-1144374; SC0018297; 00009650; AC03-76SF00098
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 477; Journal Issue: 3; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; stars; supernovae

Citation Formats

Vartanyan, David, Burrows, Adam, Radice, David, Skinner, M. Aaron, and Dolence, Joshua. Revival of the fittest: exploding core-collapse supernovae from 12 to 25 M⊙. United States: N. p., 2018. Web. doi:10.1093/mnras/sty809.
Vartanyan, David, Burrows, Adam, Radice, David, Skinner, M. Aaron, & Dolence, Joshua. Revival of the fittest: exploding core-collapse supernovae from 12 to 25 M⊙. United States. doi:10.1093/mnras/sty809.
Vartanyan, David, Burrows, Adam, Radice, David, Skinner, M. Aaron, and Dolence, Joshua. Wed . "Revival of the fittest: exploding core-collapse supernovae from 12 to 25 M⊙". United States. doi:10.1093/mnras/sty809.
@article{osti_1441344,
title = {Revival of the fittest: exploding core-collapse supernovae from 12 to 25 M⊙},
author = {Vartanyan, David and Burrows, Adam and Radice, David and Skinner, M. Aaron and Dolence, Joshua},
abstractNote = {Here, we present results of 2D axisymmetric core-collapse supernova simulations, employing the FORNAX code, of nine progenitor models spanning 12 to 25 M⊙. Four of the models explode with inelastic scattering off electrons and neutrons as well as the many-body correction to neutrino-nucleon scattering opacities. We show that these four models feature sharp Si–O interfaces in their density profiles, and that the corresponding dip in density reduces the accretion rate around the stalled shock and prompts explosion. The non-exploding models lack such a steep feature, highlighting the Si–O interface as one key to explosion. Furthermore, we show that all of the non-exploding models can be nudged to explosion with modest changes to macrophysical inputs, including moderate rotation and perturbations to infall velocities, as well as to microphysical inputs, including reasonable changes to neutrino-nucleon interaction rates, suggesting that all the models are perhaps close to criticality. Exploding models have energies of a few × 1050 erg at the end of our simulation, and are rising, emphasizing the need to continue these simulations over larger grids and for longer times to reproduce the energies seen in nature. Morphology of the explosion contributes to the explosion energy, with more isotropic ejecta producing larger explosion energies. We do not find evidence for the Lepton-number Emission Self-sustained Asymmetry. Finally, we look at proto-neutron star (PNS) properties and explore the role of dimension in our simulations. We find that convection in the PNS produces larger PNS radii as well as greater ‘νμ’ luminosities in 2D compared to 1D.},
doi = {10.1093/mnras/sty809},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 477,
place = {United States},
year = {Wed Mar 28 00:00:00 EDT 2018},
month = {Wed Mar 28 00:00:00 EDT 2018}
}

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