NEUTRINO-DRIVEN EXPLOSION OF A 20 SOLAR-MASS STAR IN THREE DIMENSIONS ENABLED BY STRANGE-QUARK CONTRIBUTIONS TO NEUTRINO–NUCLEON SCATTERING

By T. Melson, Hans-Thomas Janka, R. Bollig, Florian Hanke, Andreas Marek, Bernhard Müller. 2015

166 citations recorded by the source corpus.

Interactions with neutrons and protons play a crucial role for the neutrino opacity of matter in the supernova core. Their current implementation in many simulation codes, however, is rather schematic and ignores not only modifications for the correlated nuclear medium of the nascent neutron star, but also free-space corrections from nucleon recoil, weak magnetism, or strange quarks, which can easily add up to changes of several 10% for neutrino energies in the spectral peak. In the Garching supernova simulations with the Prometheus-Vertex code, such sophistications have been included for a long time except for the strange-quark contributions to the nucleon spin, which affect neutral-current neutrino scattering. We demonstrate on the basis of a 20 M ⊙ ?> progenitor star that a moderate strangeness-dependent contribution of g a s = − 0.2 ?> to the axial-vector coupling constant g a ≈ 1.26 ?> can turn an unsuccessful three-dimensional (3D) model into a successful explosion. Such a modification is in the direction of current experimental results and reduces the neutral-current scattering opacity of neutrons, which dominate in the medium around and above the neutrinosphere. This leads to increased luminosities and mean energies of all neutrino species and strengthens the neutrino-energy deposition in the heating layer. Higher nonradial kinetic energy in the gain layer signals enhanced buoyancy activity that enables the onset of the explosion at ∼300 ms after bounce, in contrast to the model with vanishing strangeness contributions to neutrino–nucleon scattering. Our results demonstrate the close proximity to explosion of the previously published, unsuccessful 3D models of the Garching group.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f48fe3b8c4ae65bb08ddd35ef84ac5af384a9676

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Citations in the corpus

Exploring Fundamentally Three-dimensional Phenomena in High-fidelity Simulations of Core-collapse Supernovae (2018, unknown): “(Hanke et al. 2013; Melson et al. 2015b,a; Lentz et al. 2015; Roberts et al. 2016; Ott et al. 2018; Summa et al. 2018).”
A TWO-PARAMETER CRITERION FOR CLASSIFYING THE EXPLODABILITY OF MASSIVE STARS BY THE NEUTRINO-DRIVEN MECHANISM (2015, background): “…to the progress in 2D and 3D modeling and in particular also through improvements in the treatment of the crucial neutrino physics and transport in collapsing stellar cores (see, e.g., Janka et al. 2012; Janka 2012; Burrows 2013; Mezzacappa et al. 2015; Melson et al. 2015, and references therein).”
Revisiting Supernova 1987A constraints on dark photons (2016, result): “Two new elements in our calculation, compared to previous work, are that (2)In fact, a neutrino burst that sustains an explosive front compatible with the observed energetics is challenging [39, 40] (though not impossible [41, 42]) to obtain in numerical simulations, and it is possible that the expl”
A simple approach to the supernova progenitor–explosion connection (2016, background): “Furthermore, in some multi-D simulations (Marek & Janka 2009 ; M¨uller et al. 2012a; Lentz et al. 2015 ; Melson et al.2015b), shock revival is delayed considerably beyond the infall of the Si/O interface and is instead triggered by a continuing improvement of the heating conditions due to the…”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, methodology): “…of Fornax are: 1) it does not employ the simplifying “ray-by-ray” approximation used by many others (Tamborra et al. 2014; Lentz et al. 2015; Melson et al. 2015; Müller 2015; Takiwaki et al. 2016; Müller et al. 2017; Summa et al. 2018) that suppresses the important lateral transport…”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, methodology): “…possible ingredients for more robust neutrino-driven explosions have recently been explored, including rapid rotation (Janka et al. 2016; Takiwaki et al. 2016) and a reduction of neutralcurrent neutrino-nucleon scattering opacities (Melson et al. 2015b; Horowitz et al. 2017; Burrows et al. 2016).”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, methodology): “Except for low-energy explosions from the least massive progenitors (Melson et al. 2015a; Müller et al. 2018), self-consistent 3D models cannot yet follow neutrino-driven explosions sufficiently far to obtain fully converged explosion energies and remnant properties.”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “…unaffordable, general-relativistic 3D simulations of CCSNe with stateof-the-art neutrino physics have been recently performed by a number of groups (Melson et al. 2015b,a; Lentz et al. 2015; Müller et al. 2017; Ott et al. 2017; see also Takiwaki et al. 2012; Ott et al. 2013; Takiwaki et al. 2014;…”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “Moreover, Müller et al. (2016a) simulated the entire sphere using an overset Yin-Yang grid (Kageyama & Sato 2004; Wongwathanarat et al. 2010) as implemented (with some improvements) in the Prometheus supernova code (Melson 2013; Melson et al. 2015a).”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “Although such scenarios are plausible, given the large explosion asymmetries seen in recent 3D SN models (e.g., Melson et al. 2015a; Lentz et al. 2015; Müller 2016), a direct numerical demonstration of NS kicks beyond 1000 km s−1 by the gravitational tug-boat mechanism in 3D SN simulations is…”
THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATED USING A 15 M⊙ PROGENITOR (2015, background): “The 3D simulations of the Garching group (Hanke et al. 2013; Tamborra et al. 2013, 2014; Melson et al. 2015a) all exhibit declining Rshock that are only (temporarily) reversed by sharp declines in accretion.”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, unknown): “…neutrino-radiation-hydrodynamics simulations of CCSNe have become available in the past several years (Tamborra et al. 2013; Lentz et al. 2015; Melson et al. 2015a, 2015b; Roberts et al. 2016; Müller et al. 2017; Glas et al. 2019; Kuroda et al. 2018; O’Connor & Couch 2018; Ott et al. 2018;…”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, background): “Additionally,the exploding20M (cid:2) model s20s (Melson et al. 2015b, with a mod-iﬁed axial-vector coupling constant for neutral current scattering) illustrates changes in the GW signal in exploding models.”
A successful 3D core-collapse supernova explosion model (2018, methodology): “Later, this group (Melson et al. 2015a) witnessed the explosion of a zero-metallicity 9.6-”