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Title: The Progenitor Dependence of Core-collapse Supernovae from Three-dimensional Simulations with Progenitor Models of 12–40 M

Journal Article · · The Astrophysical Journal. Letters (Online)
ORCiD logo [1]; ORCiD logo [2];  [3];  [4];  [5]; ORCiD logo [6]
  1. Kyoto Univ. (Japan); California Inst. of Technology (CalTech), Pasadena, CA (United States)
  2. Michigan State Univ., East Lansing, MI (United States)
  3. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  4. Kyoto Univ. (Japan)
  5. Univ. of Illinois, Urbana-Champaign, IL (United States)
  6. Perimeter Inst. for Theoretical Physics, Waterloo, ON (Canada); Univ. of Guelph, ON (Canada); Louisiana State Univ., Baton Rouge, LA (United States)

We present a first study of the progenitor star dependence of the three-dimensional (3D) neutrino mechanism of core-collapse supernovae. We employ full 3D general-relativistic multi-group neutrino radiation-hydrodynamics and simulate the postbounce evolutions of progenitors with zero-age main sequence masses of 12, 15, 20, 27, and 40 M. All progenitors, with the exception of the 12 M ⊙ star, experience shock runaway by the end of their simulations. In most cases, a strongly asymmetric explosion will result. We demonstrate three qualitatively distinct evolutions that imply a complex dependence of explosion dynamics on progenitor density structure, neutrino heating, and 3D flow. (1) Progenitors with massive cores, shallow density profiles, and high post-core-bounce accretion rates experience very strong neutrino heating and neutrino-driven turbulent convection, leading to early shock runaway. Accretion continues at a high rate, likely leading to black hole formation. (2) Intermediate progenitors experience neutrino-driven, turbulence-aided explosions triggered by the arrival of density discontinuities at the shock. These occur typically at the silicon/silicon–oxygen shell boundary. (3) Progenitors with small cores and density profiles without strong discontinuities experience shock recession and develop the 3D standing-accretion shock instability (SASI). Shock runaway ensues late, once declining accretion rate, SASI, and neutrino-driven convection create favorable conditions. These differences in explosion times and dynamics conclude in a non-monotonic relationship between progenitor and compact remnant mass.

Research Organization:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Organization:
USDOE Office of Science (SC), Basic Energy Sciences (BES). Scientific User Facilities Division
Grant/Contract Number:
AC02-05CH11231; CAREER PHY-1151197; PHY-1404569; OAC-1550514; AST-1333520
OSTI ID:
1524172
Journal Information:
The Astrophysical Journal. Letters (Online), Vol. 855, Issue 1; ISSN 2041-8213
Publisher:
Institute of Physics (IOP)Copyright Statement
Country of Publication:
United States
Language:
English
Citation Metrics:
Cited by: 80 works
Citation information provided by
Web of Science

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Cited By (25)

The impact of different neutrino transport methods on multidimensional core-collapse supernova simulations journal November 2018
A successful 3D core-collapse supernova explosion model journal September 2018
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors journal January 2019
Temporal and angular variations of 3D core-collapse supernova emissions and their physical correlations journal August 2019
Three-dimensional supernova explosion simulations of 9-, 10-, 11-, 12-, and 13-M⊙ stars journal February 2019
A full general relativistic neutrino radiation-hydrodynamics simulation of a collapsing very massive star and the formation of a black hole journal April 2018
Long-term simulations of multi-dimensional core-collapse supernovae: Implications for neutron star kicks journal August 2019
Progenitor Mass Distribution of Core-collapse Supernova Remnants in Our Galaxy and Magellanic Clouds Based on Elemental Abundances journal August 2018
Parallelized Solution Method of the Three-dimensional Gravitational Potential on the Yin–Yang Grid journal August 2018
Hydrodynamical Neutron-star Kicks in Electron-capture Supernovae and Implications for the CRAB Supernova journal September 2018
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae journal September 2018
PUSHing Core-collapse Supernovae to Explosions in Spherical Symmetry. II. Explodability and Remnant Properties journal December 2018
Three-dimensional Core-collapse Supernova Simulations with Multidimensional Neutrino Transport Compared to the Ray-by-ray-plus Approximation journal March 2019
Pulsational Pair-instability Supernovae in Very Close Binaries journal August 2019
Neutrino-driven Instability of Ion Acoustic Waves in an Ultrarelativistic Degenerate Plasma journal October 2019
Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae journal November 2019
Resolution Study for Three-dimensional Supernova Simulations with the Prometheus-Vertex Code journal March 2020
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae journal April 2019
Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae text January 2018
A Successful 3D Core-Collapse Supernova Explosion Model text January 2018
Three-Dimensional Core-Collapse Supernova Simulations with Multi-Dimensional Neutrino Transport Compared to the Ray-by-Ray-plus Approximation text January 2018
Characterizing the Gravitational Wave Signal from Core-Collapse Supernovae text January 2018
Effects of the standing accretion-shock instability and the lepton-emission self-sustained asymmetry in the neutrino emission of rotating supernovae text January 2019
Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M$_{\odot}$ Stars text January 2019
Long-term Simulations of Multi-Dimensional Core-collapse Supernovae: Implications for Neutron Star Kicks text January 2019

Figures / Tables (7)