The Overarching Framework of Core-Collapse Supernova Explosions as Revealed by 3D Fornax Simulations

TL;DR

This study presents the largest set of 3D core-collapse supernova simulations, revealing diverse explosion outcomes, morphological features, and nucleosynthetic implications across a broad range of progenitor masses.

Contribution

It provides new insights into supernova explodability, morphology, and nucleosynthesis by analyzing nineteen detailed 3D simulations across various progenitors.

Findings

Most models explode, but some do not, indicating explodability varies.

Explosion energy correlates with progenitor mass, with higher-mass stars producing more energetic explosions.

Inner ejecta are mostly neutron-rich with a proton-rich tail, affecting nucleosynthesis.

Abstract

We have conducted nineteen state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the "compactness" measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular vis \`a vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Y$_e = 0.5$, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.