Core-collapse supernovae

TL;DR

Core-collapse supernovae are explosive stellar endpoints that play a crucial role in cosmic element enrichment, with complex physical processes and diverse observational phenomena that inform stellar evolution and high-energy astrophysics.

Contribution

This paper provides a comprehensive review of core-collapse supernovae, covering their evolution, explosion mechanisms, observational features, and remnants, highlighting current open questions and future research directions.

Findings

Core-collapse supernovae produce key elements like oxygen, neon, and silicon.

Their light curves and spectra reveal insights into stellar evolution and nucleosynthesis.

Supernova remnants like Cas A and Crab Nebula offer detailed 3D structural information.

Abstract

Core-collapse supernovae (CCSNe) are the explosive end-points of stellar evolution for $M_{ZAMS} \gtrsim 8$ $M_\odot$ stars. The cores of these stars collapse to neutron stars, a process in which high neutrino luminosity drives off the overlying stellar layers, which get ejected with thousands of kilometers per second. These supernovae enrich their host galaxies with elements made both during the star's life and in the explosion, providing the main cosmic source of elements such as oxygen, neon and silicon. Their high luminosities ($\sim$ $10^{42}$ erg s$^{-1}$ at peak) make SNe beacons to large distances, and their light curves and spectra provide rich information on single and binary stellar evolution, nucleosynthesis, and a diverse set of high-energy physical processes. As the SN ejecta sweep up circumstellar and interstellar matter, it eventually enters a supernova remnant phase, exemplified by nearby, spatially resolved remnants such as Cas A and the Crab Nebula. In this phase, shocks and pulsar winds continue to light up the interior of the exploded stars, giving detailed information about their 3D structure. We review the central concepts of CCSNe, from the late stages of evolution of massive stars, through collapse, explosion, and electromagnetic display, to the final remnant phase. We briefly discuss still open questions, and current and future research avenues.