The Deaths of Very Massive Stars

TL;DR

This paper reviews the evolution and death of very massive stars over 30 solar masses, discussing their diverse outcomes, nucleosynthesis, and significance in cosmic history.

Contribution

It provides a comprehensive overview of the theoretical models and possible end states of very massive stars, emphasizing the effects of initial conditions and physics assumptions.

Findings

Massive stars can produce a wide range of supernova brightnesses.

They can form black holes, gamma-ray bursts, or collapse quietly.

Their nucleosynthesis spans from CNO elements to iron group.

Abstract

The theory underlying the evolution and death of stars heavier than 10 Msun on the main sequence is reviewed with an emphasis upon stars much heavier than 30 Msun. These are stars that, in the absence of substantial mass loss, are expected to either produce black holes when they die, or, for helium cores heavier than about 35 Msun, encounter the pair instability. A wide variety of outcomes is possible depending upon the initial composition of the star, its rotation rate, and the physics used to model its evolution. These heavier stars can produce some of the brightest supernovae in the universe, but also some of the faintest. They can make gamma-ray bursts or collapse without a whimper. Their nucleosynthesis can range from just CNO to a broad range of elements up to the iron group. Though rare nowadays, they probably played a disproportionate role in shaping the evolution of the universe following the formation of its first stars.