Explosion Mechanisms of Core-Collapse Supernovae

By Hans-Thomas Janka. 2012

929 citations recorded by the source corpus.

Supernova theory, numerical and analytic, has made remarkable progress in the past decade. This progress was made possible by more sophisticated simulation tools, especially for neutrino transport, improved microphysics, and deeper insights into the role of hydrodynamic instabilities. Violent, large-scale nonradial mass motions are generic in supernova cores. The neutrino-heating mechanism, aided by nonradial flows, drives explosions, albeit low-energy ones, of O-Ne-Mg-core and some Fe-core progenitors. The characteristics of the neutrino emission from newborn neutron stars were revised, new features of the gravitational-wave signals were discovered, our notion of supernova nucleosynthesis was shattered, and our understanding of pulsar kicks and explosion asymmetries was significantly improved. But simulations also suggest that neutrino-powered explosions might not explain the most energetic supernovae and hypernovae, which seem to demand magnetorotational driving. Now that modeling is being advanced from...

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/eb404c853fa60841568920ba39e4c99b14f65016

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Citations in the corpus

A simple approach to the supernova progenitor–explosion connection (2016, methodology): “Neither the assumption of a constant, time-independent binding energy (M¨uller & Janka 2015), nor the assumption that e g scales with the gravitational potential energy at the shock (Janka 2012) provides an optimal ﬁt to simulation results.”
Stellar cooling bounds on new light particles: plasma mixing effects (2016, background): “the review [22]), and impose the simple ‘Raffelt bound’ approximation on the energy loss from new particles.”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “…is arguably the neutrinodriven mechanism, which relies on the partial reabsorption of neutrinos emitted from the young proto-neutron star (PNS) and the accretion layer at its surface to revive the shock and power the explosion (for reviews, see Mezzacappa 2005; Janka 2012; Burrows et al. 2012).”
The Long-Baseline Neutrino Experiment: Exploring Fundamental Symmetries of the Universe (2013, background): “The infall is followed by a bounce when sufficiently high core density is reached, and in some unknown (but nonzero) fraction of cases, the shock wave formed after the bounce results in a bright explosion [195].”
Theoretical Challenges in Galaxy Formation (2016, background): “During these singular and final events in a massive star’s live typically 2 - 5 M of gas are ejected into the ambient interstellar medium (ISM) at supersonic velocities of veject ∼ 6000 − 7000kms−1 (Janka 2012) driving a shock into the ambient ISM.”
NEUTRINO-DRIVEN EXPLOSION OF A 20 SOLAR-MASS STAR IN THREE DIMENSIONS ENABLED BY STRANGE-QUARK CONTRIBUTIONS TO NEUTRINO–NUCLEON SCATTERING (2015, background): “…neutrino heating above the gain radius initiates the outward acceleration of the stalled bounce shock and provides a major fraction of the energy that unbinds the explosion ejecta and powers the SN blast wave (e.g., Colgate & White 1966; Bethe & Wilson 1985; Bethe 1990; Janka 2012; Burrows 2013).”
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout (2014, background): “Current state-of-the-art simulations of neutrino-driven CCSN predict that hydrodynamic instabilities play a crucial role in the explosion mechanism that leads to the ejection of the stellar mantle and envelope of exploding massive stars (see, e.g., Janka 2012, for a recent review).”
Symmetry energy impact in simulations of core-collapse supernovae (2013, background): “an be relevant under supernova conditions. PACS. 2 6.60.-c 26.60.Kp 97.60.Bw 1 Introduction Stars more massive than roughly 8 times the mass of our sun (M) end their life as core-collapse supernovae [1,2]. These are triggered by the contraction of the stellar core as degenerate electrons are capture”
Neutrino Mass Ordering from Oscillations and Beyond: 2018 Status and Future Prospects (2018, background): “…limits, the eventual detection of supernovae neutrinos will still provide precious information about the details of the explosion process (see e.g., Janka, 2012; Mirizzi et al., 2016; Scholberg, 2018 and references therein), and also of neutrino mixing effects in dense media, see also Horiuchi and…”
Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, background): “As the SN is not spherically symmetric, the explosion usually leads to a kick imparted on the newborn compact remnant (Janka 2012).”
Non-Radial Instabilities and Progenitor Asphericities in Core-Collapse Supernovae (2014, methodology): “While the small effect of perturbations with high ` is thus relatively easy to understand, the case of perturbations with ` = 1 presents something of a conundrum.”
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 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).”