Nucleosynthesis from massive stars 50 years after B2FH

TL;DR

This review discusses how mass loss and rotation influence massive star evolution and nucleosynthesis, emphasizing the role of fast-rotating metal-poor stars, or 'spinstars', in explaining various astrophysical phenomena and early Universe ionization.

Contribution

It introduces the concept of 'spinstars'—fast-rotating, very metal-poor stars—and explores their impact on nucleosynthesis and cosmic evolution, a novel perspective in stellar astrophysics.

Findings

Mass loss dominates at high metallicity.

Rotation is key at low metallicity.

Spinstars may explain primary nitrogen and early Universe ionization.

Abstract

We review some important observed properties of massive stars. Then we discuss how mass loss and rotation affect their evolution and help in giving better fits to observational constraints. Consequences for nucleosynthesis at different metallicities are discussed. Mass loss appear to be the key feature at high metallicity, while rotation is likely dominant at low and very low metallicities. We discuss various indications supporting the view that very metal poor stars had their evolution strongly affected by rotational mixing. Many features, like the origin of primary nitrogen at low metallicity, that of the C-rich extremely metal poor halo stars, of He-rich stars in massive globular clusters, of the O-Na anticorrelation in globular clusters may be related to the existence of a population of very fast rotating metal poor stars that we tentatively call the {\it spinstars}. A fraction of these {\it spinstars} may also be the progenitors of GRB in very metal poor regions. They may avoid pair instability explosion due to the heavy mass loss undergone during their early evolutionary phases and be, dependent on their frequency, important sources of ionising photons in the early Universe.