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

Ott, Christian D.; Roberts, Luke F.; da Silva Schneider, André; Fedrow, Joseph M.; Haas, Roland; Schnetter, Erik

doi:10.3847/2041-8213/aaa967

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

Journal Article · 26 February 2018 · The Astrophysical Journal. Letters (Online)

DOI: https://doi.org/10.3847/2041-8213/aaa967 · OSTI ID:1524172

^[1];

^[2]; da Silva Schneider, André ^[3]; Fedrow, Joseph M. ^[4]; Haas, Roland ^[5];

^[6]

Kyoto Univ. (Japan); California Inst. of Technology (CalTech), Pasadena, CA (United States)
Michigan State Univ., East Lansing, MI (United States)
California Inst. of Technology (CalTech), Pasadena, CA (United States)
Kyoto Univ. (Japan)
Univ. of Illinois, Urbana-Champaign, IL (United States)
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.

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Research Organization:: Lawrence Berkeley National Laboratory (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

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Characterizing the Gravitational Wave Signal from Core-Collapse Supernovae Radice, David; Morozova, Viktoriya; Burrows, Adam arXiv https://doi.org/10.48550/arxiv.1812.07703	text	January 2018
Effects of the standing accretion-shock instability and the lepton-emission self-sustained asymmetry in the neutrino emission of rotating supernovae Walk, Laurie; Tamborra, Irene; Janka, Hans-Thomas arXiv https://doi.org/10.48550/arxiv.1901.06235	text	January 2019
Three-Dimensional Supernova Explosion Simulations of 9-, 10-, 11-, 12-, and 13-M$_{\odot}$ Stars Burrows, Adam; Radice, David; Vartanyan, David arXiv https://doi.org/10.48550/arxiv.1902.00547	text	January 2019
Long-term Simulations of Multi-Dimensional Core-collapse Supernovae: Implications for Neutron Star Kicks Nakamura, Ko; Takiwaki, Tomoya; Kotake, Kei arXiv https://doi.org/10.48550/arxiv.1904.08088	text	January 2019