Three-dimensional core-collapse supernova simulated using a 15 $M_\odot$ progenitor

TL;DR

This study presents 3D and 2D simulations of a 15 solar mass core-collapse supernova, revealing that 3D explosions are delayed compared to 2D, with differences in plume development and shock revival timing.

Contribution

First ab initio 3D and 2D neutrino radiation hydrodynamics simulations of a 15 solar mass supernova from core bounce to explosion.

Findings

3D explosions are delayed by ~100 ms compared to 2D.

Explosion growth is slower in 3D.

Large-angle plumes lead to shock revival in 3D.

Abstract

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 $M_\odot$ progenitor through 440 ms after core bounce. Both 3D and 2D models achieve explosions, however, the onset of explosion (shock revival) is delayed by $\sim$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 $\sim$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.