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

Understand

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.