Explosions of O-Ne-Mg cores, the Crab supernova, and subluminous type II-P supernovae

By Francisco-Shu Kitaura, Hans-Thomas Janka, W. Hillebrandt. 2005

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We present results of simulations of stellar collapse and explosions in spherical symmetry for progenitor stars in the 8–$10\,M_\odot$ range with an O-Ne-Mg core. The simulations were continued until nearly one second after core bounce and were performed with the Prometheus/Vertex code with a variable Eddington factor solver for the neutrino transport, including a state-of-the-art treatment of neutrino-matter interactions. Particular effort was made to implement nuclear burning and electron capture rates with sufficient accuracy to ensure a smooth continuation, without transients, from the progenitor evolution to core collapse. Using two different nuclear equations of state (EoSs), a soft version of the Lattimer & Swesty EoS and the significantly stiffer Wolff & Hillebrandt EoS, we found no prompt explosions, but instead delayed explosions, powered by neutrino heating and the neutrino-driven baryonic wind which sets in about 200 ms after bounce. The models eject little nickel (${<} 0.015~M_\odot$), explode with an energy of ${\ga}0.1\times 10^{51}\,$erg, and leave behind neutron stars (NSs) with a baryonic mass near $1.36\,M_\odot$. Different from previous models of such explosions, the ejecta during the first second have a proton-to-baryon ratio of $Y_{\rm{e}} \ga 0.46$, which suggests a chemical composition that is not in conflict with galactic abundances. No low-entropy matter with $Y_{\rm{e}} \ll 0.5$ is ejected. This excludes such explosions as sites of a low-entropy r-process. The low explosion energy and nucleosynthetic implications are compatible with the observed properties of the Crab supernova, and the small nickel mass supports the possibility that our models explain some subluminous type II-P supernovae.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/970f99e30d64654ef47a1ec6d16ee81703299e2e

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Citations in the corpus

CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, methodology): “Spherically symmetric, first-principles simulations do not yield explosions by the neutrino-driven mechanism except for low-mass progenitors with oxygen–neon–magnesium cores (Kitaura et al. 2006; Janka et al. 2008) or small iron cores (Melson et al. 2015).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, methodology): “From the work of Kitaura et al. (2006), Buras et al. (2006b), and Janka et al. (2005ab) one might conclude that the neutrino mechanism requires compact cores and tenuous outer envelopes, but that for such progenitors a solely neutrino-driven explosion is perforce weak.”
NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2011, background): “Explosions in spherical symmetry have been obtained only for the low mass 8.8 M⊙ O–Ne–Mg core from Nomoto (1983, 1984, 1987) by Kitaura et al. (2006) and Fischer et al. (2010).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, background): “While fully self-consistent spherically symmetric simulations generally fail to explode in all but a few very low mass progenitors (cf. Kitaura et al. 2006; Burrows et al. 2007a), one can explode any star by the 1D neutrino mechanism by artificially increasing the energy deposition in the postshock…”
Formation of Double Neutron Star Systems (2017, background): “Given the somewhat narrow mass window for producing EC SNe (Podsiadlowski et al. 2004), it is likely that Fe CCSNe dominate the formation rate of lowmass NSs. Detailed population synthesis studies are needed to answer this (Kruckow et al. 2017, in prep.).”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, background): “Today there is a universal consensus in supernova theory that the neutrino-driven explosion mechanism hinges vitally on the supporting action of multidimensional hydrodynamic instabilities (with the notable exception of low-mass progenitors with O-Ne-Mg core; Kitaura et al. 2006).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “9M⊙), called the O-Ne-Mg or electron capture supernova (e.g., Kitaura et al. 2006; Janka et al. 2008; Wanajo et al. 2009, 2011).”
Two-Dimensional Multiangle, Multigroup Neutrino Radiation-Hydrodynamic Simulations of Postbounce Supernova Cores (2008, background): “Yet, weak explosions may be obtained in 1D for the lowest mass progenitors, O-Ne-Mg cores (Kitaura et al. 2006; Burrows et al. 2007a).”
A successful 3D core-collapse supernova explosion model (2018, background): “Only the rare progenitors at the lowest ZAMS masses with very steep density profiles exterior to the collapsing Chandrasekhar core explode in spherical symmetry (Kitaura et al. 2006; Burrows et al. 2007c; Radice et al. 2018).”
Formation and evolution of compact binaries in globular clusters – II. Binaries with neutron stars (2007, background): “The explosion energy of such an event is significantlylower than that inferred for core-collapse supernovae (Dessart et l. 2006; Kitaura et al. 2006).”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, methodology): “Effects of Convection A potentially important effect that is lacking in the one-dimensional simulations of Kitaura et al. (2006) is convective mixing of the ejecta (see the results of a twodimensional simulation of a collapsing O-Ne-Mg core in Janka et al. 2008b).”
SN 2005cs in M51 – II. Complete evolution in the optical and the near-infrared (2009, background): “…need to understand whether all underluminous SNe IIP are generated by the explosion of moderate-mass stars (e.g. electon capture supernovae, see Kitaura et al. 2006; Wanajo et al. 2008), or if some of them are instead related to black-hole forming massive precursors as suggested by Zampieri et…”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “In contrast, low-mass progenitors with ONeMg cores and iron cores are expected to explode with low energies of at most around 1050 erg (Kitaura et al. 2006; Dessart et al. 2006; Janka et al. 2012; Melson et al. 2015b).”
Symmetry energy impact in simulations of core-collapse supernovae (2013, background): “ simulations, which include threeavor Boltzmann neutrino transport and a detailed nuclear equation of state (EOS), obtain explosions in spherical symmetry only for low-mass progenitor stars with 8 9M [7,8]. This is related to the special structure of such progenitors. Their low-mass core of about 1:”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, background): “…in 1D, 2D, or 3D, because the most detailed 1D models generically fail to explode, except for the lowest mass progenitors (Rampp & Janka 2000; Bruenn et al. 2001; Liebendörfer et al. 2001; Mezzacappa et al. 2001; Thompson et al. 2003; Kitaura et al. 2006; Janka et al. 2008; Suwa et al. 2014).”