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Title: A successful 3D core-collapse supernova explosion model

Abstract

In this paper, we present the results of our three-dimensional, multigroup, multineutrino-species radiation/hydrodynamic simulation using the state-of-the-art code FORNAX of the terminal dynamics of the core of a non-rotating 16 M⊙ stellar progenitor. The calculation incorporates redistribution by inelastic scattering, a correction for the effect of many-body interactions on the neutrino–nucleon scattering rates, approximate general relativity (including the effects of gravitational redshifts), velocity-dependent frequency advection, and an implementation of initial perturbations in the progenitor core. The model explodes within ~100 ms of bounce (near when the silicon–oxygen interface is accreted through the temporarily stalled shock) and by the end of the simulation (here, ~677 ms after bounce) is accumulating explosion energy at a rate of ~2.5 × 10 50 erg s -1. The supernova explodes with an asymmetrical multiplume structure, with one hemisphere predominating. The gravitational mass of the residual proto-neutron star at ~677 ms is ~1.42 M . Even at the end of the simulation, explosion in most of the solid angle is accompanied by some accretion in an annular region at the wasp-like waist of the debris field. The ejecta electron fraction (Y e) is distributed between ~0.48 and ~0.56, with most of the ejecta mass proton-rich. Thismore » may have implications for supernova nucleosynthesis, and could have a bearing on the p- and νp-processes and on the site of the first peak of the r-process. The ejecta spatial distributions of both Ye and mass density are predominantly in wide-angle plumes and large-scale structures, but are nevertheless quite patchy« less

Authors:
ORCiD logo [1];  [1]; ORCiD logo [2];  [3]; ORCiD logo [4]
  1. Princeton Univ., NJ (United States)
  2. Princeton Univ., NJ (United States); Inst. for Advanced Study, Princeton, NJ (United States)
  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.:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC); Univ. of California, San Diego, CA (United States); Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States); Univ. of California, Oakland, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC); USDOE Laboratory Directed Research and Development (LDRD) Program
OSTI Identifier:
1479117
Alternate Identifier(s):
OSTI ID: 1543971; OSTI ID: 1571594
Report Number(s):
LA-UR-18-28730
Journal ID: ISSN 0035-8711
Grant/Contract Number:  
AC03-76SF00098; AC52-06NA25396; AC52-07NA27344; SC0018297; 00009650; LA-UR-18-28730; 89233218CNA000001
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 482; Journal Issue: 1; 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 C. A successful 3D core-collapse supernova explosion model. United States: N. p., 2018. Web. doi:10.1093/mnras/sty2585.
Vartanyan, David, Burrows, Adam, Radice, David, Skinner, M. Aaron, & Dolence, Joshua C. A successful 3D core-collapse supernova explosion model. United States. doi:10.1093/mnras/sty2585.
Vartanyan, David, Burrows, Adam, Radice, David, Skinner, M. Aaron, and Dolence, Joshua C. Mon . "A successful 3D core-collapse supernova explosion model". United States. doi:10.1093/mnras/sty2585.
@article{osti_1479117,
title = {A successful 3D core-collapse supernova explosion model},
author = {Vartanyan, David and Burrows, Adam and Radice, David and Skinner, M. Aaron and Dolence, Joshua C.},
abstractNote = {In this paper, we present the results of our three-dimensional, multigroup, multineutrino-species radiation/hydrodynamic simulation using the state-of-the-art code FORNAX of the terminal dynamics of the core of a non-rotating 16 M⊙ stellar progenitor. The calculation incorporates redistribution by inelastic scattering, a correction for the effect of many-body interactions on the neutrino–nucleon scattering rates, approximate general relativity (including the effects of gravitational redshifts), velocity-dependent frequency advection, and an implementation of initial perturbations in the progenitor core. The model explodes within ~100 ms of bounce (near when the silicon–oxygen interface is accreted through the temporarily stalled shock) and by the end of the simulation (here, ~677 ms after bounce) is accumulating explosion energy at a rate of ~2.5 × 1050 erg s-1. The supernova explodes with an asymmetrical multiplume structure, with one hemisphere predominating. The gravitational mass of the residual proto-neutron star at ~677 ms is ~1.42 M⊙. Even at the end of the simulation, explosion in most of the solid angle is accompanied by some accretion in an annular region at the wasp-like waist of the debris field. The ejecta electron fraction (Ye) is distributed between ~0.48 and ~0.56, with most of the ejecta mass proton-rich. This may have implications for supernova nucleosynthesis, and could have a bearing on the p- and νp-processes and on the site of the first peak of the r-process. The ejecta spatial distributions of both Ye and mass density are predominantly in wide-angle plumes and large-scale structures, but are nevertheless quite patchy},
doi = {10.1093/mnras/sty2585},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 1,
volume = 482,
place = {United States},
year = {2018},
month = {9}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
DOI: 10.1093/mnras/sty2585

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