New Neutron-Capture Site in Massive Pop III and Pop II Stars as a Source for Heavy Elements in the Early Galaxy

TL;DR

This paper introduces a new neutron-capture process in early massive stars, explaining the origin of heavy elements like Sr and Ba in the early Galaxy and the observed abundance patterns in very metal-poor stars.

Contribution

It proposes a novel neutron-capture site in early stars caused by proton ingestion, providing a unified explanation for heavy element formation in the early universe.

Findings

Explains the ubiquity of Sr and Ba in the early Galaxy.

Accounts for heavy element patterns in very metal-poor stars.

Proposes a single site for multiple neutron-capture processes.

Abstract

We propose a new neutron-capture site in early metal-poor and metal-free stars of $\sim 20$--$30 \,\mathrm{M}_\odot$ that results from proton ingestion in the He shell during late stages of the stars' lives. Most of the neutron capture occurs in the first $\lesssim 10^6\,$s following proton ingestion when $^{13}{\rm C}(\alpha,\mathrm{n})^{16}\mathrm{O}$ produces neutron densities typical of the intermediate neutron-capture process. This phase may be followed by another lasting $\gtrsim 10^7\,$s with $^{17}\mathrm{O}(\alpha,\mathrm{n})^{20}\mathrm{Ne}$ producing much lower neutron densities typical of the slow neutron-capture process. We explore the dependence of the proposed neutron-capture nucleosynthesis on the amount and time of proton ingestion, the initial metallicity, and the ensuing supernova shock. We obtain a range of heavy element abundance patterns including those attributed to the slow neutron-capture process or a combination of the slow and rapid neutron-capture processes. Our results can account for the observed ubiquity of heavy elements such as Sr and Ba in the early Galaxy and explain puzzling abundance patterns of these elements in at least some very metal-poor (VMP) stars including those of the carbon-enhanced varieties. In the latter case, the explanation by the single site proposed here differs from the existing paradigm that attributes various classes of VMP stars to enrichment by multiple different sites.