Modeling Core-Collapse Supernovae in Three Dimensions

By Chris L. Fryer, M. Warren. 2002

173 citations recorded by the source corpus.

We present the first complete three-dimensional simulations of the core collapse of a massive star from the onset of collapse to the resultant supernova explosion. We compare the structure of the convective instabilities that occur in three-dimensional models with those of past two-dimensional simulations. Although the convective instabilities are clearly three-dimensional in nature, we find that both the size scale of the flows and the net enhancement to neutrino heating does not differ greatly between two- and three-dimensional models. The explosion energy, explosion timescale, and remnant mass does not differ by more than 10% between two- and three-dimensional simulations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/336a057695ed8dfa0780238675e72f041c7e3422

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Citations in the corpus

The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “Before 3D modelling began in earnest (leaving aside tentative sallies into 3D by Fryer & Warren 2002), it was hoped that 3D effects might facilitate shock revival even at earlier times than in 2D, and that this might then also provide a solution to the energy problem, since more energy can be…”
NEW TWO-DIMENSIONAL MODELS OF SUPERNOVA EXPLOSIONS BY THE NEUTRINO-HEATING MECHANISM: EVIDENCE FOR DIFFERENT INSTABILITY REGIMES IN COLLAPSING STELLAR CORES (2012, background): “Convection also appears to be the “primary” instability in the 3D models of Fryer & Warren (2002) and in recent 2D and 3D simulations based on different implementations of a simple light-bulb approximation (Murphy & Burrows 2008; Fernández & Thompson 2009a; Nordhaus et al. 2010b; Hanke et al.…”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, background): “11 Herant et al. (1994) and Fryer & Warren (2002,2004) are an exception.”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, background): “…simulations (e.g., Herant et al. 1994, Burrows et al. 1995, Janka & Müller 1996, Fryer 1999, Fryer & Heger 2000) and three-dimensional (3D) models (Fryer & Warren 2002, 2004) show the importance of convective overturn in the neutrinoheating layer behind the stalled supernova shock, which can…”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport - I. Numerical method and results for a 15 solar mass star (2005, background): “Can the positive results of previous simulations with simplified neutrino transport by grey, flux-limited diffusion (Herant et al. 1994; Fryer 1999; Fryer & Heger 2000; Fryer & Warren 2002, 2004) be confirmed?”
Neutrino-dominated Accretion and Supernovae (2005, background): “It is also unclear if the two-dimensional turbulence seen in the calculations provides a realistic description of full three-dimensional turbulence (see, e.g., Fryer & Warren 2002, 2004).”
Non-spherical core collapse supernovae - II. The late-time evolution of globally anisotropic neutrino-driven explosions and their implications for SN 1987 A (2005, background): “…2D simulations, which include spectral neutrino transport, (see Buras et al. 2003, 2006a,b) could not confirm the success of first generation models, which employed gray neutrino diffusion and found explosions (e.g. Herant et al. 1994; Burrows et al. 1995; Fryer 1999; Fryer & Warren 2002, 2004).”
High‐resolution calculations of merging neutron stars – II. Neutrino emission (2003, background): “…with externally imposed neutrino fluxes or spectra (Herant et al. 1994; Burrows, Hayes & Fryxell 1995; Janka & Müller 1996; Mezzacappa et al. 1998; Fryer & Warren 2002) make a bridge between simulation and observation, the traditional investigations in spherically symmetric geometry proceeded to…”
The Effects of Binary Evolution on the Dynamics of Core Collapse and Neutron Star Kicks (2003, background): “Prompt (fast) explosions and supernova kicks At present, neither the mechanism that produces a successful core-collapse supernova nor the origin of supernova kicks is properly understood (see Janka et al. 2003; Fryer 2003 for detailed recent reviews, and also Fryer & Warren (2002, 2003)).”
THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVA SIMULATED USING A 15 M⊙ PROGENITOR (2015, background): “Earlier work by Fryer & Warren (2002, 2004) using non-spectral νRHD found explosions in 2D and 3D to be similar.”
COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, background): “Our alternate convection-enhanced supernova engine model focuses on strong convective models developing rapidly and driving an explosion within the first 250 ms (e.g., Herant et al. 1994; Fryer & Warren 2002).”
On the Determination of Ejecta Structure and Explosion Asymmetry from the X-Ray Knots of Cassiopeia A (2003, background): “Additionally, the generic problem of core-collapse simulation producing too much neutron-rich matter appears to be slightly exacerbated, though Fryer & Warren (2002) caution that much of the input physics upon which this conclusion depends is still uncertain.”
SELF-SUSTAINED ASYMMETRY OF LEPTON-NUMBER EMISSION: A NEW PHENOMENON DURING THE SUPERNOVA SHOCK-ACCRETION PHASE IN THREE DIMENSIONS (2014, background): “…stalled shock was predicted by Bethe (1990) and confirmed by the first 2D hydrodynamical simulations (Herant et al. 1992; Herant et al. 1994; Burrows et al. 1995; Miller et al. 1993; Janka & Müller 1995, 1996; Mezzacappa et al. 1998) as well as in three dimensions (3D; Fryer & Warren 2002, 2004).”
Multidimensional supernova simulations with approximative neutrino transport. I. Neutron star kicks and the anisotropy of neutrino-driven explosions in two spatial dimensions (2006, background): “This effect may have been the reason why low-mode instabilities were not found to be dominant in the 3D simulations of Fryer & Warren (2002, 2004), which developed explosions on rather short time scales after bounce.”