Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport - I. Numerical method and results for a 15 solar mass star

By R. Buras, Markus Rampp, Hans-Thomas Janka, K. K. M. F. A. Garching, Mpi Munich. 2005

347 citations recorded by the source corpus.

Supernova models with a full spectral treatment of the neutrino transport are presented, employing the prometheus/vertex neutrino-hydrodynamics code with a variable Eddington factor closure of the ${\cal O}(v/c)$ moments equations of neutrino number, energy, and momentum. Our “ray-by-ray plus” approximation developed for two- (or three-) dimensional problems assumes that the local neutrino distribution function is azimuthally symmetric around the radial direction, which implies that the nonradial flux components disappear. Other terms containing the angular velocity components are retained in the moments equations and establish a coupling of the transport at different latitudes by lateral derivatives. Also lateral components of the neutrino pressure gradients are included in the hydrodynamics equations. This approximative approach for neutrino transport in multi-dimensional environments is motivated and critically assessed with respect to its capabilities, limitations, and inaccuracies in the context of supernova simulations. In this first paper of a series, one- (1D) and two-dimensional (2D) core-collapse calculations for a (nonrotating) $15~\ensuremath{M_{\odot}}$ star are discussed, uncertainties in the treatment of the equation of state – numerical and physical – are tested, Newtonian results are compared with simulations using a general relativistic potential, bremsstrahlung and interactions of neutrinos of different flavors are investigated, and the standard approximation in neutrino-nucleon interactions with zero energy transfer is replaced by rates that include corrections due to nucleon recoil, thermal motions, weak magnetism, and nucleon correlations. Models with the full implementation of the “ray-by-ray plus” spectral transport were found not to explode, neither in spherical symmetry nor in 2D when the computational grid is constrained to a lateral wedge ( ± $45\degr$) around the equator. The success of previous two-dimensional simulations with grey, flux-limited neutrino diffusion can therefore not be confirmed. An explosion is obtained in 2D for the considered $15~\ensuremath{M_{\odot}}$ progenitor, when the radial velocity terms in the neutrino momentum equation are omitted. This manipulation increases the neutrino energy density in the convective gain layer by about 20-30% and thus the integral neutrino energy deposition in this region by about a factor of two compared to the non-exploding 2D model with the full transport. The spectral treatment of the transport and detailed description of charged-current processes leads to proton-rich neutrino-heated ejecta, removing the problem that previous explosion models with approximate neutrino treatment overproduced $N=50$ closed neutron shell nuclei by large factors.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/629f81d6dbcd57dc8f21b7a80da02112f0a1ee99

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Citations in the corpus

Nucleosynthesis-relevant conditions in neutrino-driven supernova outflows. I. Spherically symmetric (2006, methodology): “…not consistently account for the reverse shock, which is a hydrodynamical feature found in several simulations (e.g., Janka & Müller 1995; Janka & Müller 1996; Article published by EDP Sciences A160, page 1 of 13 Burrows et al. 1995; Buras et al. 2006b; Arcones et al. 2007; Fischer et al. 2010).”
Simulations of Magnetically Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation (2007, methodology): “There is an emerging consensus that the core-collapse supernovamechanism is essentially aspherical and that instabilities and the breaking of spherical symmetry are keys to explosion (Buras et al. 2006a, 2006b; Burrows et al. 2006, 2007; Blondin et al. 2003).”
COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, background): “Most current studies of core-collapse supernovae have focused on a neutrino-driven engine enhanced by convection above the proto-NS surface (Herant et al. 1994; Fryer & Warren 2004; Buras et al. 2006; Burrows et al. 2006; Fryer & Young 2007; Scheck et al. 2008; Bruenn et al. 2009).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, methodology): “M⊙ model of WHW02 boasts the thinnest mantle of their whole model set, and this is consistent with the explanation given in §1 for why Buras et al. (2006b) obtained a SASI- and neutrino-aided explosion, albeit weak, but no such explosion for the more massive cores with shallower and thicker density…”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “In fact, a recent twodimensional simulation with a more massive progenitor (15 M⊙, Buras et al. 2006) shows that the bulk of the ejecta turns out to be proton-rich (Ye > 0.5).”
Nucleosynthesis in Early Supernova Winds. II. The Role of Neutrinos (2005, methodology): “Our fiducial model for exploring nucleosynthesis in the protonrich wind is the explosion of a 15 M star (Janka et al. 2003; Buras et al. 2006).”
The Spin Periods and Rotational Profiles of Neutron Stars at Birth (2005, background): “Such velocity terms are deemed to be of relative importance by the Garching group, who find neutrino-driven explosions when turning them off (Rampp & Janka 2002; Buras et al. 2003, 2006).”
SASI ACTIVITY IN THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF SUPERNOVA CORES (2013, methodology): “…code with detailed ray-by-rayplus neutrino transport and the sophisticated treatment of energy-dependent neutrino interactions also applied in previous 2D simulations with this code (e.g., Buras et al. 2006b; Marek & Janka 2009) and in the 2D GR models of Müller et al. (2012b,a, 2013).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, background): “Buras et al. (2006b) who also artificially exploded this progenitor in 1D, though with much more sophisticated neutrino transport, find2 an average heating efficiency of 0.1−0.15 which is consistent with our result.”
Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, methodology): “According to the recent explosion calculations with the neutrino effect (e.g., Rampp & Janka 2000; Buras et al. 2006b), materials with large Ye ( 0.54) may be ejected.”
Two-dimensional hydrodynamic core-collapse supernova simulations with spectral neutrino transport II. Models for different progenitor stars (2005, methodology): “For our two-dimensional studies with assumed azimuthal symmetry we used the numerical code, input physics, and resolution as described in Buras et al. (2006) and specified in Table1.”