Stellar winds and metal enrichment from fast-rotating Population III stars

TL;DR

This paper investigates how stellar winds from fast-rotating Population III stars contribute to early metal enrichment and the formation of carbon-enhanced metal-poor stars, combining wind feedback with supernovae in a semi-analytical model.

Contribution

It introduces a semi-analytical model exploring the combined effects of Pop III stellar winds and supernovae on early chemical enrichment, explaining observed CEMP-no star patterns.

Findings

Predicted carbon and iron abundance patterns match observations of CEMP-no stars.

Wind-driven enrichment can produce extremely iron-poor, carbon-enhanced stars.

Both wind+ISM accretion and faint supernova scenarios can explain CEMP-no stars.

Abstract

Stellar winds from fast-rotating Population III (Pop III) stars have long been suspected to make important contributions to early metal enrichment, as features in the nucleosynthesis of such `spinstars' are consistent with the chemical abundance patterns of some metal-poor stars in the local Universe. Particularly, stellar winds rich in light elements can provide another pathway towards explaining the carbon enhancement in carbon-enhanced metal-poor (CEMP) stars. In this work, we focus on the feedback of Pop III stellar winds combined with supernovae (SNe), and derive the resulting chemical signatures in the enriched medium. We explore a large parameter space of Pop III star formation, feedback, yields from winds and SNe with a semi-analytical model. The predicted pattern of carbon and iron abundances of second-generation stars agrees well with observations of CEMP-no stars ($[\rm Ba/Fe]<0$) at $[\rm Fe/H]\lesssim -3$ and $A(\mathrm{C})\lesssim 7$, under the optimistic assumption of significant mass loss by winds from massive ($\gtrsim 25\ \rm M_{\odot}$) stars that collapse into BHs without SNe. In this scenario, carbon-rich but iron-free second-generation stars can form in systems dominated by enrichment from winds, gaining trace amounts of iron by accretion from the interstellar medium, to become the most iron-poor and carbon-enhanced stars seen in observations ($[\rm Fe/H]\lesssim -4$, $[\rm C/Fe]\gtrsim 2$). We conclude that the observed CEMP-no stars can be explained by both our winds + ISM accretion channel as well as the well-studied faint SN scenario. Wind feedback from Pop~III spinstars deserves more detailed modelling in early cosmic structure formation.