TY - JOUR
T1 - Electron-capture and Low-mass Iron-core-collapse Supernovae
T2 - New Neutrino-radiation-hydrodynamics Simulations
AU - Radice, David
AU - Burrows, Adam
AU - Vartanyan, David
AU - Skinner, M. Aaron
AU - Dolence, Joshua C.
N1 - Funding Information:
Support was provided by the Max-Planck/Princeton Center (MPPC) for Plasma Physics (NSF PHY-1523261). D.R. gratefully acknowledges support from the Schmidt Fellowship. A.B. acknowledges support from the NSF under award number AST-1714267. J.D. acknowledges support from a Laboratory Directed Research and Development Early Career Research award at LANL. 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 by 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. The authors express their gratitude to Ted Barnes of the DOE Office of Nuclear Physics for facilitating their use of NERSC
Funding Information:
The authors acknowledge Chuck Horowitz, Evan O’Connor, and Todd Thompson for productive conversations, concerning insight into and help with the microphysics, and Ernazar Abdikamalov, Sean M.Couch, Luke F.Roberts, and Christian D.Ott for fruitful discussions on the nature of core-collapse supernovae. Support was provided by the Max-Planck/Princeton Center (MPPC) for Plasma Physics (NSF PHY-1523261). D.R. gratefully acknowledges support from the Schmidt Fellowship. A.B. acknowledges support from the NSF under award number AST-1714267. J.D. acknowledges support from a Laboratory Directed Research and Development Early Career Research award at LANL. 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 by 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. The authors express their gratitude to Ted Barnes of the DOE Office of Nuclear Physics for facilitating their use of NERSC. This paper has been assigned a LANL preprint # LAUR-17-20973.
Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/11/20
Y1 - 2017/11/20
N2 - We present new 1D (spherical) and 2D (axisymmetric) simulations of electron-capture (EC) and low-mass iron-corecollapse supernovae (SN). We consider six progenitor models: the ECSN progenitor from Nomoto; two ECSN-like low-mass low-metallicity iron-core progenitors from A. Heger (2016, private communication); and the 9, 10, and 11 M (zero-age main-sequence) progenitors from Sukhbold et al. We confirm that the ECSN and ESCN-like progenitors explode easily even in 1D with explosion energies of up to a 0.15 Bethes (1 B ≡ 1051 erg), and are a viable mechanism for the production of very-low-mass neutron stars. However, the 9, 10, and 11 M progenitors do not explode in 1D and are not even necessarily easier to explode than higher-mass progenitor stars in 2D. We study the effect of perturbations and of changes to the microphysics and we find that relatively small changes can result in qualitatively different outcomes, even in 1D, for models sufficiently close to the explosion threshold. Finally, we revisit the impact of convection below the protoneutron star (PNS) surface. We analyze 1D and 2D evolutions of PNSs subject to the same boundary conditions. We find that the impact of PNS convection has been underestimated in previous studies and could result in an increase of the neutrino luminosity by up to factors of two.
AB - We present new 1D (spherical) and 2D (axisymmetric) simulations of electron-capture (EC) and low-mass iron-corecollapse supernovae (SN). We consider six progenitor models: the ECSN progenitor from Nomoto; two ECSN-like low-mass low-metallicity iron-core progenitors from A. Heger (2016, private communication); and the 9, 10, and 11 M (zero-age main-sequence) progenitors from Sukhbold et al. We confirm that the ECSN and ESCN-like progenitors explode easily even in 1D with explosion energies of up to a 0.15 Bethes (1 B ≡ 1051 erg), and are a viable mechanism for the production of very-low-mass neutron stars. However, the 9, 10, and 11 M progenitors do not explode in 1D and are not even necessarily easier to explode than higher-mass progenitor stars in 2D. We study the effect of perturbations and of changes to the microphysics and we find that relatively small changes can result in qualitatively different outcomes, even in 1D, for models sufficiently close to the explosion threshold. Finally, we revisit the impact of convection below the protoneutron star (PNS) surface. We analyze 1D and 2D evolutions of PNSs subject to the same boundary conditions. We find that the impact of PNS convection has been underestimated in previous studies and could result in an increase of the neutrino luminosity by up to factors of two.
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U2 - 10.3847/1538-4357/aa92c5
DO - 10.3847/1538-4357/aa92c5
M3 - Article
AN - SCOPUS:85038900304
SN - 0004-637X
VL - 850
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 43
ER -