Progenitors of core-collapse supernovae

TL;DR

This review summarizes recent advances in identifying progenitor stars of core-collapse supernovae, highlighting the initial mass thresholds, different progenitor types, and the implications for stellar evolution and explosion mechanisms.

Contribution

It consolidates recent observational findings on supernova progenitors, clarifies the initial mass ranges, and discusses the diversity of progenitor types and their explosion outcomes.

Findings

Minimum progenitor mass for supernovae is about 8 solar masses.

Most type Ibc supernovae originate from moderate-mass binary systems.

Highly energetic broad-lined Ic supernovae likely come from Wolf-Rayet stars.

Abstract

Knowledge of the progenitors of core-collapse supernovae is a fundamental component in understanding the explosions. The recent progress in finding such stars is reviewed. The minimum initial mass that can produce a supernova has converged to 8 +/- 1 solar masses, from direct detections of red supergiant progenitors of II-P SNe and the most massive white dwarf progenitors, although this value is model dependent. It appears that most type Ibc supernovae arise from moderate mass interacting binaries. The highly energetic, broad-lined Ic supernovae are likely produced by massive, Wolf-Rayet progenitors. There is some evidence to suggest that the majority of massive stars above ~20 solar masses may collapse quietly to black-holes and that the explosions remain undetected. The recent discovery of a class of ultra-bright type II supernovae and the direct detection of some progenitor stars bearing luminous blue variable characteristics suggests some very massive stars do produce highly energetic explosions. The physical mechanism is open to debate and these SNe pose a challenge to stellar evolutionary theory.