First Stars. II. Evolution with mass loss

TL;DR

This paper models the evolution of very massive Population III stars with mass loss, exploring how initial mass, metallicity, and mass loss influence their evolution, nucleosynthesis, and final fate, including supernova types.

Contribution

It introduces a study of mass loss effects on Population III star evolution across various masses and metallicities, highlighting their potential roles in cosmic reionization and element enrichment.

Findings

Low metallicity stars are hotter, more compact, and luminous.

Mass loss leads to efficient mixing of nucleosynthetic products.

Final outcomes include pair-instability supernovae or hypernovae.

Abstract

The first stars are assumed to be predominantly massive. Although, due to the low initial abundances of heavy elements the line-driven stellar winds are supposed to be inefficient in the first stars, these stars may loose a significant amount of their initial mass by other mechanisms. In this work, we study the evolution with a prescribed mass loss rate of very massive, galactic and pregalactic, Population III stars, with initial metallicities $Z=10^{-6}$ and $Z=10^{-9}$, respectively, and initial masses 100, 120, 150, 200, and 250$\,M_{\odot}$ during the hydrogen and helium burning phases. The evolution of these stars depends on their initial mass, metallicity and the mass loss rate. Low metallicity stars are hotter, compact and luminous, and they are shifted to the blue upper part in the Hertzprung-Russell diagram. With mass loss these stars provide an efficient mixing of nucleosynthetic products, and depending on the He-core mass their final fate could be either pair-instability supernovae or energetic hypernovae. These stars contributed to the reionization of the universe and its enrichment with heavy elements, which influences the subsequent star formation properties.