THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATED USING A 15 M⊙ PROGENITOR

By E. Lentz, S. Bruenn, W. Hix, A. Mezzacappa, O. E. Bronson Messer, E. Endeve, J. Blondin, J. A. Harris, P. Marronetti, K. Yakunin. 2015

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We have performed ab initio neutrino radiation hydrodynamics simulations in three and two spatial dimensions (3D and 2D) of core-collapse supernovae from the same 15 M☉ progenitor through 440 ms after core bounce. Both 3D and 2D models achieve explosions; however, the onset of explosion (shock revival) is delayed by ∼100 ms in 3D relative to the 2D counterpart and the growth of the diagnostic explosion energy is slower. This is consistent with previously reported 3D simulations utilizing iron-core progenitors with dense mantles. In the ∼100 ms before the onset of explosion, diagnostics of neutrino heating and turbulent kinetic energy favor earlier explosion in 2D. During the delay, the angular scale of convective plumes reaching the shock surface grows and explosion in 3D is ultimately lead by a single, large-angle plume, giving the expanding shock a directional orientation not dissimilar from those imposed by axial symmetry in 2D simulations. We posit that shock revival and explosion in the 3D simulation may be delayed until sufficiently large plumes form, whereas such plumes form more rapidly in 2D, permitting earlier explosions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/e2287f427af8be0d54b6d17571ac4dbfdfc4e93d

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Citations in the corpus

Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “…few models have been evolved sufficiently far by other groups to show the emerging explosion geometry (Takiwaki et al. 2014; Melson et al. 2015a,b; Lentz et al. 2015; Ott et al. 2018; Vartanyan et al. 2018), and although there is a preponderance of unipolar explosions, examples of more bipolar…”
A successful 3D core-collapse supernova explosion model (2018, methodology): “Our method of deresolving near the polar axis for 3D simulations allows us to partially overcome axial artifacts seen conventionally in 3D simulations in spherical coordinates (see, e.g. Lentz et al. 2015; Müller et al. 2017).”
Characterizing the Gravitational Wave Signal from Core-collapse Supernovae (2018, unknown): “…number of sophisticated 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;…”
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…”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, methodology): “…group are characterised by more optimistic heating conditions, larger average shock radii, and higher kinetic energies in non-spherical motions compared to 2D for extended periods of time; the same is true for the delayed (compared to 2D) 3D explosion of Lentz et al. (2015) of a 15M progenitor.”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, methodology): “…3D simulations of explosions with three-ﬂavour multigroup neutrino transport, culminating in the recent models of the Garching and Oak Ridge groups (Lentz et al. 2015; Melson, Janka & Marek 2015a; Melson et al. 2015b) with their rigorous treatment of the transport and neutrino micro-physics in…”
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).”
The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, methodology): “To summarize, the advantages 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…”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, methodology): “…various algorithms for multi-group neutrino transport ranging from the very rigorous Vertex (Hanke et al. 2013; Melson et al. 2015a,b; Janka et al. 2016) and Chimera (Lentz et al. 2015) models to more approximate methods (Takiwaki et al. 2012, 2014, 2016; Müller 2015; Roberts et al. 2016).”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, background): “…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; Müller 2015; Roberts…”
What can be learned from a future supernova neutrino detection (2017, background): “The general trend of greater difficulty of exploding a star in 3D compared to 2D (and also that the difference depends upon whether dynamics are convection or SASI dominated) is also seen in the more sophisticated simulations including neutrino transport [148, 39, 149] but, in one case, once the sta”
A simple approach to the supernova progenitor–explosion connection (2016, background): “…remnant mass distribution for several reasons: despite recent successes in 3D explosion modelling (Melson, Janka & Marek 2015a ; Melson et al. 2015b; Lentz et al. 2015 ; M¨uller 2015), obtaining explosions has proved more difﬁcult in 3D multigroup neutrino transport models than in 2D (Hanke et…”