TY - JOUR
T1 - The Progenitor Dependence of Core-collapse Supernovae from Three-dimensional Simulations with Progenitor Models of 12-40 Mo
AU - Ott, Christian D.
AU - Roberts, Luke F.
AU - Da Silva Schneider, André
AU - Fedrow, Joseph M.
AU - Haas, Roland
AU - Schnetter, Erik
N1 - Funding Information:
This research was partially supported by NSF grants CAREER PHY-1151197, PHY-1404569, OAC-1550514, and AST-1333520, and the Sherman Fairchild Foundation. The simulations took over a year to complete and were carried out on (10,000) compute cores of NSF/NCSA Blue Waters (PRAC ACI-1440083, OCI-0725070 and ACI-1238993, and Illinois allocation baov), of Edison at the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, and of the Texas Advanced Computing Center Stampede and Stampede2 clusters under NSF XSEDE allocation TG-PHY100033. This article has been assigned Yukawa Institute for Theoretical Physics report No. YITP-17-122.
Funding Information:
We acknowledge helpful discussions with D.Radice, H.Nagakura, Y.Suwa, K. Kiuchi, M.Shibata, J.Takeda, H.-T.Janka, R.Bollig, M.Obergaulinger, S.Couch, E. O’Connor, P.Mösta, and K. S.Thorne. This research was partially supported by NSF grants CAREER PHY-1151197, PHY-1404569, OAC-1550514, and AST-1333520, and the Sherman Fairchild Foundation. The simulations took over a year to complete and were carried out on (10,000) compute cores of NSF/NCSA Blue Waters (PRAC ACI-1440083, OCI-0725070 and ACI-1238993, and Illinois allocation baov), of Edison at the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, and of the Texas Advanced Computing Center Stampede and Stampede2 clusters under NSF XSEDE allocation TG-PHY100033. This article has been assigned Yukawa Institute for Theoretical Physics report No.YITP-17-122.
Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved.
PY - 2018/3/1
Y1 - 2018/3/1
N2 - 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 o. All progenitors, with the exception of the 12 M o star, experience shock runaway by the end of their simulations. In most cases, a strongly asymmetric explosion will result. We find three qualitatively distinct evolutions that suggest 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 result in a non-monotonic relationship between progenitor and compact remnant mass.
AB - 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 o. All progenitors, with the exception of the 12 M o star, experience shock runaway by the end of their simulations. In most cases, a strongly asymmetric explosion will result. We find three qualitatively distinct evolutions that suggest 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 result in a non-monotonic relationship between progenitor and compact remnant mass.
KW - neutrinos
KW - stars: black holes
KW - stars: neutron
KW - supernovae: general
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U2 - 10.3847/2041-8213/aaa967
DO - 10.3847/2041-8213/aaa967
M3 - Article
AN - SCOPUS:85043483854
SN - 2041-8205
VL - 855
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L3
ER -