Physics of massive stars relevant for the modeling of Wolf-Rayet populations

TL;DR

This paper examines the physical processes influencing massive star evolution, focusing on differences in rotational models and the effects of mass loss in single and binary systems.

Contribution

It compares two types of rotating models and assesses how mass loss impacts the evolution of massive stars in different configurations.

Findings

Differences between models with and without angular momentum transport.

Mass loss significantly affects the evolution of massive stars.

Impacts are notable in both single and binary star evolution.

Abstract

Key physical ingredients governing the evolution of massive stars are mass losses, convection and mixing in radiative zones. These effects are important both in the frame of single and close binary evolution. The present paper addresses two points: 1) the differences between two families of rotating models, i.e. the family of models computed with and without an efficient transport of angular momentum in radiative zones; 2) The impact of the mass losses in single and in close binary models.