The Progenitor Dependence of Core-collapse Supernovae from Three-dimensional Simulations with Progenitor Models of 12–40 M ⊙
Abstract
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.more »
- Authors:
-
[1];
[2];
[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)
- Publication Date:
- Research Org.:
- Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Basic Energy Sciences (BES). Scientific User Facilities Division
- OSTI Identifier:
- 1524172
- Grant/Contract Number:
- AC02-05CH11231; CAREER PHY-1151197; PHY-1404569; OAC-1550514; AST-1333520
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal. Letters (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal. Letters (Online); Journal Volume: 855; Journal Issue: 1; Journal ID: ISSN 2041-8213
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; neutrinos; stars: black holes; stars: neutron; supernovae: general
Citation Formats
Ott, Christian D., Roberts, Luke F., da Silva Schneider, André, Fedrow, Joseph M., Haas, Roland, and Schnetter, Erik. The Progenitor Dependence of Core-collapse Supernovae from Three-dimensional Simulations with Progenitor Models of 12–40 M ⊙. United States: N. p., 2018.
Web. doi:10.3847/2041-8213/aaa967.
Ott, Christian D., Roberts, Luke F., da Silva Schneider, André, Fedrow, Joseph M., Haas, Roland, & Schnetter, Erik. The Progenitor Dependence of Core-collapse Supernovae from Three-dimensional Simulations with Progenitor Models of 12–40 M ⊙. United States. https://doi.org/10.3847/2041-8213/aaa967
Ott, Christian D., Roberts, Luke F., da Silva Schneider, André, Fedrow, Joseph M., Haas, Roland, and Schnetter, Erik. Mon .
"The Progenitor Dependence of Core-collapse Supernovae from Three-dimensional Simulations with Progenitor Models of 12–40 M ⊙". United States. https://doi.org/10.3847/2041-8213/aaa967. https://www.osti.gov/servlets/purl/1524172.
@article{osti_1524172,
title = {The Progenitor Dependence of Core-collapse Supernovae from Three-dimensional Simulations with Progenitor Models of 12–40 M ⊙},
author = {Ott, Christian D. and Roberts, Luke F. and da Silva Schneider, André and Fedrow, Joseph M. and Haas, Roland and Schnetter, Erik},
abstractNote = {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.},
doi = {10.3847/2041-8213/aaa967},
journal = {The Astrophysical Journal. Letters (Online)},
number = 1,
volume = 855,
place = {United States},
year = {2018},
month = {2}
}
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Figures / Tables:
Figure-1: Density as a function of enclosed mass coordinate for our set of progenitor stars. The density profile is the single most important progenitor property since it sets the postbounce accretion rate. Note that the structures inside ∼1.3–1.4 M⊙ obey a homology relationship due to the universal nature of degeneratemore »
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