Supernova Nucleosynthesis in the Early Universe

TL;DR

This paper investigates how different types of Population III supernovae contributed to the early universe's metal enrichment by comparing nucleosynthesis yields with the observed abundance patterns of extremely metal-poor stars.

Contribution

It introduces models of jet-induced supernovae with varying energies and explores their nucleosynthesis yields across different stellar masses, linking them to observed stellar abundances.

Findings

Higher [C/Fe] ratios are associated with lower [Fe/H] in EMP stars.

Varieties of Pop III supernovae can explain the observed abundance trends.

The models reproduce the diversity in elemental abundance patterns of EMP stars.

Abstract

The first metal enrichment in the universe was made by supernova (SN) explosions of population (Pop) III stars. The trace remains in abundance patterns of extremely metal-poor (EMP) stars. We investigate the properties of nucleosynthesis in Pop III SNe by means of comparing their yields with the abundance patterns of the EMP stars. We focus on (1) jet-induced SNe with various energy deposition rates [$\dot{E}_{\rm dep}=(0.3-1500)\times10^{51}{\rm ergs s^{-1}}$], and (2) SNe of stars with various main-sequence masses ($M_{\rm ms}=13-50M_\odot$) and explosion energies [$E=(1-40)\times10^{51}$ergs]. The varieties of Pop III SNe can explain varieties of the EMP stars: (1) higher [C/Fe] for lower [Fe/H] and (2) trends of abundance ratios [X/Fe] against [Fe/H].