Evolution and Final Fates of a Rotating 25 M$_{\odot}$ Pop III star

TL;DR

This paper models the evolution and final outcomes of two rotating 25 solar mass Population III stars, highlighting how rotation influences mass loss and supernova characteristics.

Contribution

It presents the first detailed 1D stellar evolution models of rotating Pop III stars with different initial rotation rates, emphasizing rotational effects on mass loss and supernovae.

Findings

Rapid rotation causes significant surface enrichment and mass loss.

Rotational mixing impacts the star's evolution and explosion properties.

Simulated light curves illustrate differences in supernova outcomes.

Abstract

In this proceeding, we present the 1-dimensional stellar evolution of two rotating population III (Pop III) star models, each having a mass of 25 M$_{\odot}$ at the zero-age main-sequence (ZAMS). The slowly rotating model has an initial angular rotational velocity of 10 per cent of the critical angular rotational velocity. In contrast, the rapidly rotating model has an initial angular rotational velocity of 70 per cent of the critical angular rotational velocity. As an effect of rotationally enhanced mixing, we find that the rapidly rotating model suffers an enormous mass loss due to the deposition of a significant amount of CNO elements toward the surface after the main-sequence phase. We also display the simulated light curves as these models explode into core-collapse supernovae (CCSNe).