The Status of Multi-Dimensional Core-Collapse Supernova Models

By Bernhard Müller. Publications Astronomical Society of Australia, 2016

187 citations recorded by the source corpus.

Abstract Models of neutrino-driven core-collapse supernova explosions have matured considerably in recent years. Explosions of low-mass progenitors can routinely be simulated in 1D, 2D, and 3D. Nucleosynthesis calculations indicate that these supernovae could be contributors of some lighter neutron-rich elements beyond iron. The explosion mechanism of more massive stars remains under investigation, although first 3D models of neutrino-driven explosions employing multi-group neutrino transport have become available. Together with earlier 2D models and more simplified 3D simulations, these have elucidated the interplay between neutrino heating and hydrodynamic instabilities in the post-shock region that is essential for shock revival. However, some physical ingredients may still need to be added/improved before simulations can robustly explain supernova explosions over a wide range of progenitors. Solutions recently suggested in the literature include uncertainties in the neutrino rates, rotation, and seed perturbations from convective shell burning. We review the implications of 3D simulations of shell burning in supernova progenitors for the ‘perturbations-aided neutrino-driven mechanism,’ whose efficacy is illustrated by the first successful multi-group neutrino hydrodynamics simulation of an 18 solar mass progenitor with 3D initial conditions. We conclude with speculations about the impact of 3D effects on the structure of massive stars through convective boundary mixing.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/e2683116d2c61730f23afba31bd0d223e722a3a5

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Citations in the corpus

A successful 3D core-collapse supernova explosion model (2018, background): “H E ] 1 3 Se p Burrows (2013), Müller (2016), and Janka et al. (2016).”
Stellar cooling bounds on new light particles: plasma mixing effects (2016, background): “han SN limits for masses . 50keV. However, SN limits apply up to masses ˘100MeV. It should be emphasised that there is still signicant uncertainty regarding the behaviour of core-collapse supernovae [19], with con icting models in the literature of even the very basic energy source involved [20]. As”
Neutron Star Kicks by the Gravitational Tug-boat Mechanism in Asymmetric Supernova Explosions: Progenitor and Explosion Dependence (2016, background): “…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…”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, background): “…these two indispensable ingredients – neutrino heating and cooling and three-dimensional (3D) fluid flow – with a high degree of confidence have become available during the last few years (see Janka et al. 2016 and Müller 2016 for an overview of recent results and simulation methodologies).”
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.”