Post-explosion evolution of core-collapse supernovae

TL;DR

This study uses 2D hydrodynamical simulations with simplified neutrino physics to analyze the post-explosion evolution of core-collapse supernovae, revealing how early shock revival influences final explosion outcomes and the variability of neutrino-driven winds.

Contribution

It provides a comprehensive analysis of post-explosion supernova evolution across different progenitors, rotation rates, and neutrino efficiencies, highlighting the impact of early shock revival on explosion properties.

Findings

Early shock revival determines final explosion energy and remnant mass.

Late-time mass accretion can increase explosion energy.

Neutrino-driven winds are not guaranteed after all successful explosions.

Abstract

We investigate the post-explosion phase in core-collapse supernovae with 2D hydrodynamical simulations and a simple neutrino treatment. The latter allows us to perform 46 simulations and follow the evolution of the 32 successful explosions during several seconds. We present a broad study based on three progenitors (11.2 $M_\odot$, 15 $M_\odot$, and 27 $M_\odot$), different neutrino-heating efficiencies, and various rotation rates. We show that the first seconds after shock revival determine the final explosion energy, remnant mass, and properties of ejected matter. Our results suggest that a continued mass accretion increases the explosion energy even at late times. We link the late-time mass accretion to initial conditions such as rotation strength and shock deformation at explosion time. Only some of our simulations develop a neutrino-driven wind that survives for several seconds. This indicates that neutrino-driven winds are not a standard feature expected after every successful explosion. Even if our neutrino treatment is simple, we estimate the nucleosynthesis of the exploding models for the 15 $M_\odot$ progenitor after correcting the neutrino energies and luminosities to get a more realistic electron fraction.