A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations

TL;DR

This study systematically investigates proto-neutron star convection in 3D core-collapse supernova simulations, revealing its characteristics, variability, and effects on neutrino luminosities and potential pulsar magnetic field generation.

Contribution

It provides the first comprehensive 3D analysis of PNS convection in CCSN models, linking convection strength to PNS mass and exploring its impact on neutrino emission and magnetic fields.

Findings

PNS convection is common in 3D CCSN simulations.

Convection strength correlates with PNS mass, not large-scale supernova dynamics.

PNS convection enhances certain neutrino luminosities and may influence pulsar magnetic fields.

Abstract

This paper presents the first systematic study of proto-neutron star (PNS) convection in three dimensions (3D) based on our latest numerical Fornax models of core-collapse supernova (CCSN). We confirm that PNS convection commonly occurs, and then quantify the basic physical characteristics of the convection. By virtue of the large number of long-term models, the diversity of PNS convective behavior emerges. We find that the vigor of PNS convection is not correlated with CCSN dynamics at large radii, but rather with the mass of PNS $-$ heavier masses are associated with stronger PNS convection. We find that PNS convection boosts the luminosities of $\nu_{\mu}$, $\nu_{\tau}$, $\bar{\nu}_{\mu}$, and $\bar{\nu}_{\tau}$ neutrinos, while the impact on other species is complex due to a competition of factors. Finally, we assess the consequent impact on CCSN dynamics and the potential for PNS convection to generate pulsar magnetic fields.