Physical Correlations and Predictions Emerging from Modern Core-Collapse Supernova Theory

TL;DR

This study analyzes a large set of 3D core-collapse supernova simulations to identify observable correlations with progenitor structures, revealing patterns that can inform future supernova modeling and observations.

Contribution

The paper presents the largest collection of 3D supernova models to date, deriving new correlations between explosion characteristics and progenitor core properties.

Findings

Correlations between explosion energy and progenitor mantle binding energy.

Testable links between explosion energy and asymmetry measures.

Relationships between explosion properties and progenitor core compactness.

Abstract

In this paper, we derive correlations between core-collapse supernova observables and progenitor core structures that emerge from our suite of twenty state-of-the-art 3D core-collapse supernova simulations carried to late times. This is the largest such collection of 3D supernova models ever generated and allows one to witness and derive testable patterns that might otherwise be obscured when studying one or a few models in isolation. From this panoramic perspective, we have discovered correlations between explosion energy, neutron star gravitational birth masses, $^{56}$Ni and $\alpha$-rich freeze-out yields, and pulsar kicks and theoretically important correlations with the compactness parameter of progenitor structure. We find a correlation between explosion energy and progenitor mantle binding energy, suggesting that such explosions are self-regulating. We also find a testable correlation between explosion energy and measures of explosion asymmetry, such as the ejecta energy and mass dipoles. While the correlations between two observables are roughly independent of the progenitor ZAMS mass, the many correlations we derive with compactness can not unambiguously be tied to a particular progenitor ZAMS mass. This relationship depends upon the compactness/ZAMS mass mapping associated with the massive star progenitor models employed. Therefore, our derived correlations between compactness and observables may be more robust than with ZAMS mass, but can nevertheless be used in the future once massive star modeling has converged.