How Massive Single Stars End Their Life

TLDR

The fate of massive stars—whether they explode as supernovae or collapse into black holes—depends mainly on their helium core and hydrogen envelope masses, while for single stars mass loss occurs only via stellar winds that scale with metallicity. The study examines how metallicity and a simplified mass‑loss prescription influence the evolution and ultimate fate of massive stars. The authors map the dependence of remnant type and supernova class on stellar mass and metallicity, integrate over an initial mass function to predict relative populations, and speculate that rapidly rotating single stars at death could produce gamma‑ray bursts and jet‑driven supernovae.

Abstract

How massive stars die—what sort of explosion and remnant each produces—depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are the only means of mass loss, and these are a function of the metallicity of the star. We discuss how metallicity, and a simplified prescription for its effect on mass loss, affects the evolution and final fate of massive stars. We map, as a function of mass and metallicity, where black holes and neutron stars are likely to form and where different types of supernovae are produced. Integrating over an initial mass function, we derive the relative populations as a function of metallicity. Provided that single stars rotate rapidly enough at death, we speculate on stellar populations that might produce gamma-ray bursts and jet-driven supernovae.