TY - JOUR
T1 - The overarching framework of core-collapse supernova explosions as revealed by 3D FORNAX simulations
AU - Burrows, Adam
AU - Radice, David
AU - vartanyan, David
AU - Nagakura, Hiroki
AU - Skinner, M. Aaron
AU - Dolence, Joshua C.
N1 - Funding Information:
We acknowledge support from the U.S. Department of Energy Office of Science and the Office of Advanced Scientific Computing Research via the Scientific Discovery through Advanced Computing (SciDAC4) program and Grant DE-SC0018297 (subaward 00009650). In addition, we gratefully acknowledge support from the U.S. NSF under Grants AST-1714267 and PHY-1144374 [the latter via the Max-Planck/Princeton Center (MPPC) for Plasma Physics]. DR cites partial support as a Frank and Peggy Taplin Fellow at the Institute for Advanced Study. JD acknowledges support from the Laboratory Directed Research and Development program at the Los Alamos National Laboratory. Help with the equation of state (Evan O’Connor), electron capture on heavy nuclei (Gabriel Martínez-Pinedo), the initial progenitor models (Tug Sukhbold and Stan Woosley), and inelastic scattering (Todd Thompson) was provided. We thank Joe Insley of ALCF for visualization support. An award of computer time was provided by the INCITE program using Theta at the Argonne Leadership Computing Facility, which is a DOE Office of Science User Facility supported under Contract DE-AC02-06CH11357. In addition, this overall research project is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. This general
Funding Information:
project is also part of the ‘Three-Dimensional Simulations of Core-Collapse Supernovae’ PRAC allocation support by the National Science Foundation (under award #OAC-1809073). Moreover, access under the local award #TG-AST170045 to the resource Stampede2 in the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1548562, was crucial to the completion of this work. Finally, the authors employed computational resources provided by the TIGRESS High Performance Computer Center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering (PICSciE) and the Princeton University Office of Information Technology, and acknowledge our continuing allocation at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy (DOE) under contract DE-AC03-76SF00098. This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344 and has been assigned an LLNL document release number LLNL-JRNL-787982. This paper has also been assigned a LANL preprint # LA-UR-19-28512.
Funding Information:
We acknowledge support from the U.S. Department of Energy Office of Science and the Office of Advanced Scientific Computing Research via the Scientific Discovery through Advanced Computing (SciDAC4) program and Grant DE-SC0018297 (subaward 00009650). In addition, we gratefully acknowledge support from the U.S. NSF under Grants AST-1714267 and PHY-1144374 [the latter via the Max-Planck/Princeton Center (MPPC) for Plasma Physics]. DR cites partial support as a Frank and Peggy Taplin Fellow at the Institute for Advanced Study. JD acknowledges support from the Laboratory Directed Research and Development program at the Los Alamos National Laboratory. Help with the equation of state (Evan O'Connor), electron capture on heavy nuclei (Gabriel Martínez-Pinedo), the initial progenitor models (Tug Sukhbold and Stan Woosley), and inelastic scattering (Todd Thompson) was provided. We thank Joe Insley of ALCF for visualization support. An award of computer time was provided by the INCITE program using Theta at the Argonne Leadership Computing Facility, which is a DOE Office of Science User Facility supported under Contract DE-AC02-06CH11357. In addition, this overall research project is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (awards OCI-0725070 and ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. This general project is also part of the 'Three-Dimensional Simulations of Core-Collapse Supernovae' PRAC allocation support by the National Science Foundation (under award #OAC-1809073). Moreover, access under the local award #TG-AST170045 to the resource Stampede2 in the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1548562, was crucial to the completion of this work. Finally, the authors employed computational resources provided by the TIGRESS High Performance Computer Center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering (PICSciE) and the Princeton University Office of Information Technology, and acknowledge our continuing allocation at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy (DOE) under contract DE-AC03-76SF00098. This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344 and has been assigned an LLNL document release number LLNL-JRNL-787982. This paper has also been assigned a LANL preprint # LA-UR-19-28512.
Publisher Copyright:
© 2019 The Author(s).
PY - 2020/1/1
Y1 - 2020/1/1
N2 - We have conducted 19 state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the 'compactness' measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular vis à vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Ye = 0.5, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.
AB - We have conducted 19 state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the 'compactness' measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular vis à vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Ye = 0.5, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.
KW - Supernovae: general
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U2 - 10.1093/mnras/stz3223
DO - 10.1093/mnras/stz3223
M3 - Article
AN - SCOPUS:85079591604
SN - 0035-8711
VL - 491
SP - 2715
EP - 2735
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -