A Comparison of Two- And Three-Dimensional Neutrino-Hydrodynamics Simulations of Core-Collapse Supernovae

Abstract

We present numerical results on two-(2D) and three-dimensional (3D) hydrodynamic core-collapse simulations of an 11.2M ⊙ star. By changing numerical resolutions and seed perturbations systematically, we study how the postbounce dynamics is different in 2D and 3D. The calculations were performed with an energy-dependent treatment of the neutrino transport based on the isotropic diffusion source approximation scheme, which we have updated to achieve a very high computational efficiency. All the computed models in this work including nine 3D models and fifteen 2D models exhibit the revival of the stalled bounce shock, leading to the possibility of explosion. All of them are driven by the neutrino-heating mechanism, which is fostered by neutrino-driven convection and the standing-accretion-shock instability (SASI). Reflecting the stochastic nature of multi-dimensional (multi-D) neutrino-driven explosions, the blast morphology changes from models to models. However, we find that the final fate of the multi-D models whether an explosion is obtained or not, is little affected by the explosion stochasticity. In agreement with some previous studies, higher numerical resolutions lead to slower onset of the shock revival in both 3D and 2D. Based on the self-consistent supernova models leading to the possibility of explosions, our results systematically show that the revived shock expands more energetically in 2D than in 3D.

The Development of Explosions in Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12–25 Stars

“…The dynamic behavior of the accretion shock has not received the attention afforded the SASI and convection, but previous analyses using tracer particles from CHIMERA simulations has shown that much of the matter passing through the shock is directed toward the proto-NS in accretion streams (Chertkow et al 2012;Lentz et al 2012a). We notethat the one or two accretion streams that dominate the accretion in 2D simulations is not characteristic of 3D simulations, which exhibit more numerous but weaker accretion streams Tamborra et al 2013Tamborra et al , 2014Takiwaki et al 2014;Tamborra et al 2014;Abdikamalov et al 2015;Lentz et al 2015).…”

“…Zeus+IDSA is fully Newtonian and the transport omits inelastic (energy exchanging) scattering in favor of the elastic versions. Early versions neglected n mt andn mt completely, but some recent works (Nakamura et al 2015;Takiwaki et al 2014) have included a leakage scheme for these species. Suwa et al (2010) ) progenitor with a n mt -n mt leakage scheme added.…”

“…Suwa et al (2014) computed simulations for nine progenitors from Woosley & Heger (2007) including the 12, 15, and 20 M  progenitors used herein and several additional 15 M  progenitors from other authors. Among the progenitors matching our set, they found explosions for only the 12 M  progenitor, which had a diagnostic energy of 0.1 B at 600 ms after bounce and little sign of growth.…”

“…The Zeus+IDSA code (Suwa et al 2010(Suwa et al , 2013(Suwa et al , 2014Nakamura et al 2015;Takiwaki et al 2014), the VULCAN code (Dessart et al 2006;Burrows et al 2007;Ott et al 2008), and the CASTRO code (Dolence et al 2015) have been used to perform 2D simulations with Newtonian gravity, a reduced set of neutrino interactions, no relativistic neutrino transport corrections (e.g., gravitational redshift), and, in the case of Zeus+IDSA, the exclusion of muon and tau neutrinos and antineutrinos. Among all of the above efforts, VULCAN and its successor CASTRO are the only codes that implement fully 2D, rather than RbR, neutrino transport.…”

“…Three-dimensional simulations with spectral, RbR neutrino transport, approximate general relativity, and state-of-the-art weak interactions are underway, and the results from early stages of the post-bounce dynamics have been reported by Hanke et al (2013), using VERTEX, and Lentz et al (2015), using CHIMERA. Takiwaki et al (2012Takiwaki et al ( , 2014 also report 3D Newtonian simulations using Zeus +IDSA. Fully general relativistic simulations with reduced neutrino physics (a leakage scheme for neutrino transport with a reduced set of neutrino interactions)have also beenper-formed using the ZELMANI code (Ott et al 2013;Mösta et al 2014).…”