# Supernovae from massive stars

## TL;DR

This paper reviews the evolution and explosion mechanisms of massive stars (13-120 solar masses) across various metallicities and rotation speeds, highlighting how these factors influence their final fate and contributions to cosmic phenomena.

## Contribution

It provides a comprehensive overview of the presupernova evolution of massive stars considering metallicity and rotation, emphasizing their impact on stellar outcomes and cosmic evolution.

## Key findings

- Evolutionary properties influence supernova outcomes
- Mass loss, mixing, and rotation interplay affects star fate
- Final stellar fate depends on initial mass, metallicity, and rotation

## Abstract

Massive stars, by which we mean those stars exploding as core collapse supernovae, play a pivotal role in the evolution of the Universe. Therefore, the understanding of their evolution and explosion is fundamental in many branches of physics and astrophysics, among which, galaxy evolution, nucleosynthesis, supernovae, neutron stars and pulsars, black holes, neutrinos and gravitational waves. In this chapter, the author presents an overview of the presupernova evolution of stars in the range between 13 and 120 $\rm M_\odot$, with initial metallicities between [Fe/H]=-3 and [Fe/H]=0 and initial rotation velocities $\rm v=0,~150,~300~km/s$. Emphasis is placed upon those evolutionary properties that determine the final fate of the star with special attention to the interplay among mass loss, mixing and rotation. A general picture of the evolution and outcome of a generation of massive stars, as a function of the initial mass, metallicity and rotation velocity, is finally outlined.