Evolution of progenitor stars of Type Ibc supernovae and long gamma-ray bursts

TL;DR

This paper explores how rotation, binary interactions, and magnetic fields influence the evolution of massive stars leading to Type Ibc supernovae and long gamma-ray bursts, emphasizing the role of quasi-chemical homogeneity at low metallicity.

Contribution

It presents recent models of massive star evolution including rotation and binary effects, highlighting the potential similarities in progenitors and the importance of magnetic fields.

Findings

Binary and single star progenitors may not differ significantly in rotation.

Most long GRB progenitors may evolve via quasi-chemical homogeneity.

Magnetic fields could play a key role in angular momentum transport.

Abstract

We discuss how rotation and binary interactions may be related to the diversity of type Ibc supernovae and long gamma-ray bursts. After presenting recent evolutionary models of massive single and binary stars including rotation, the Tayler-Spruit dynamo and binary interactions, we argue that the nature of SNe Ibc progenitors from binary systems may not significantly differ from that of single star progenitors in terms of rotation, and that most long GRB progenitors may be produced via the quasi-chemically homogeneous evolution at sub-solar metallicity. We also briefly discuss the possible role of magnetic fields generated in the convective core of a massive star for the transport of angular momentum, which is potentially important for future stellar evolution models of supernova and GRB progenitors.