Core-collapse supernovae: Reflections and directions

By Hans-Thomas Janka, Florian Hanke, Lorenz Huedepohl, Andreas Marek, B. Mueller, M. Obergaulinger. 2012

137 citations recorded by the source corpus.

Core-collapse supernovae are among the most fascinating phenomena in astrophysics and provide a formidable challenge for theoretical investigation. They mark the spectacular end of the lives of massive stars and, in an explosive eruption, release as much energy as the sun produces during its whole life. A better understanding of the astrophysical role of supernovae as birth sites of neutron stars, black holes, and heavy chemical elements, and more reliable predictions of the observable signals from stellar death events are tightly linked to the solution of the long-standing puzzle how collapsing stars achieve to explode. In this article our current knowledge of the processes that contribute to the success of the explosion mechanism are concisely reviewed. After a short overview of the sequence of stages of stellar core-collapse events, the general properties of the progenitor-dependent neutrino emission will be briefly described. Applying sophisticated neutrino transport in axisymmetric (2D) simulations with general relativity as well as in simulations with an approximate treatment of relativistic effects, we could find successful neutrino-driven explosions for a growing set of progenitor stars. First results of three-dimensional (3D) models have been obtained, and magnetohydrodynamic simulations demonstrate that strong initial magnetic fields in the pre-collapse core can foster the onset of neutrino-powered supernova explosions even in nonrotating stars. These results are discussed in the context of the present controversy about the value of 2D simulations for exploring the supernova mechanism in realistic 3D environments, and they are interpreted against the background of the current disagreement on the question whether the standing accretion shock instability (SASI) or neutrino-driven convection is the crucial agency that supports the onset of the explosion.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1eb76dc66d9c501db90de3da5c314082a9f0f5ac

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, methodology): “The model has the merit of having been successfully exploded in 1D and multidimensional calculations (Janka et al. 2012; Melson et al. 2015), developing an explosion dynamically similar to collapsing O–Ne–Mg core progenitors (Kitaura et al. 2006; Janka et al. 2008).”
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).”
A simple approach to the supernova progenitor–explosion connection (2016, background): “…multi-group models to sufﬁciently late times to obtain saturated values for the explosion energy and remnant mass remains difﬁcult (Suwa et al. 2010; Janka et al. 2012 ; M¨uller, Janka & Marek 2012a ; M¨uller, Janka&Heger2012b;Bruennetal.2013;O’Connor&Couch2015;…”
Non-Radial Instabilities and Progenitor Asphericities in Core-Collapse Supernovae (2014, result): “…hydrodynamics simulations (Buras et al. 2006a; Marek & Janka 2009; Yakunin et al. 2010; Suwa et al. 2010; Müller, Janka & Marek 2012; Müller, Janka & Heger 2012; Janka et al. 2012; Bruenn et al. 2013; Suwa et al. 2013) has lent further credence to the idea of neutrino-driven supernova explosions.”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, methodology): “6 was first used in Janka et al. (2012), and the 3D simulation presented here is identical to the one in Müller (2016); progenitor model s11.”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, background): “…could lead to more robust and earlier explosions, not least because they may also help solve the “energy problem” in many successful 2D simulations (Janka et al. 2012; Nakamura et al. 2015; O’Connor & Couch 2015), in which the explosion energy grows rather slowly and may fall short of the…”