Ascertaining the Core Collapse Supernova Mechanism: An Emerging Picture?

TL;DR

This paper presents multi-dimensional simulations of core-collapse supernovae, revealing new insights into shock dynamics, explosion mechanisms, and the importance of three-dimensional modeling for accurate results.

Contribution

It introduces comprehensive 2D and 3D simulations showing the critical role of shock instabilities and the limitations of 2D models in supernova explosion studies.

Findings

Explosions occur when the oxygen layer accretes through the shock.

3D simulations reveal a stable m=1 SASI mode affecting angular momentum distribution.

2D models are limited by artificial symmetry constraints.

Abstract

Here we present the results from two sets of simulations, in two and three spatial dimensions. In two dimensions, the simulations include multifrequency flux-limited diffusion neutrino transport in the "ray-by-ray-plus" approximation, two-dimensional self gravity in the Newtonian limit, and nuclear burning through a 14-isotope alpha network. The three-dimensional simulations are model simulations constructed to reflect the post stellar core bounce conditions during neutrino shock reheating at the onset of explosion. They are hydrodynamics-only models that focus on critical aspects of the shock stability and dynamics and their impact on the supernova mechanism and explosion. In two dimensions, we obtain explosions (although in one case weak) for two progenitors (11 and 15 Solar mass models). Moreover, in both cases the explosion is initiated when the inner edge of the oxygen layer accretes through the shock. Thus, the shock is not revived while in the iron core, as previously discussed in the literature. The three-dimensional studies of the development of the stationary accretion shock instability (SASI) demonstrate the fundamentally new dynamics allowed when simulations are performed in three spatial dimensions. The predominant l=1 SASI mode gives way to a stable m=1 mode, which in turn has significant ramifications for the distribution of angular momentum in the region between the shock and proto-neutron star and, ultimately, for the spin of the remnant neutron star. Moreover, the three-dimensional simulations make clear, given the increased number of degrees of freedom, that two-dimensional models are severely limited by artificially imposed symmetries.