Presupernova evolution and explosive nucleosynthesis of zero metal massive stars

TL;DR

This paper introduces new zero-metallicity stellar models for stars between 13 and 80 solar masses, along with their explosive nucleosynthesis, to better understand the chemical yields of the earliest stars.

Contribution

It provides a comprehensive set of zero-metallicity stellar models and nucleosynthesis yields, extending previous work to a broader mass range and making data publicly available.

Findings

Zero-metallicity models for 13-80 solar mass stars are developed.

Comparison with metal-poor star observations supports partial fits by standard supernova yields.

The models help explain elemental abundance patterns in very metal-poor stars.

Abstract

We present a new set of zero metallicity models in the range 13-80 $\rm M_\odot$ together to the associated explosive nucleosynthesis. These models are fully homogeneous with the solar metallicity set we published in Limongi & Chieffi (2006) and will be freely available at the web site http://www.iasf-roma.inaf.it./orfeo/public{\_}html. A comparison between these yields and an average star that represents the average behavior of most of the very metal poor stars in the range $\rm -5.0<[Fe/H]<-2.5$ confirms previous findings that only a fraction of the elemental [X/Fe] may be fitted by the ejecta of $\it standard$ core collapse supernovae.