Supernova Nucleosynthesis and Extremely Metal-Poor Stars

TL;DR

This study models jet-induced supernova explosions of a primordial 40 solar mass star to explain the observed abundance patterns in extremely metal-poor stars, highlighting how explosion energy and geometry influence nucleosynthesis.

Contribution

It introduces detailed hydrodynamical and nucleosynthetic modeling of jet-induced supernovae for Population III stars, linking explosion parameters to observed stellar abundances.

Findings

Fe-peak element ejection explains EMP star patterns.

Explosion energy affects abundance diversity.

Angle-dependent yields reproduce peculiar star abundances.

Abstract

We investigate hydrodynamical and nucleosynthetic properties of the jet-induced explosion of a population III $40M_\odot$ star and compare the abundance patterns of the yields with those of the metal-poor stars. We conclude that (1) the ejection of Fe-peak products and the fallback of unprocessed materials can account for the abundance patterns of the extremely metal-poor (EMP) stars and that (2) the jet-induced explosion with different energy deposition rates can explain the diversity of the abundance patterns of the metal-poor stars. Furthermore, the abundance distribution after the explosion and the angular dependence of the yield are shown for the models with high and low energy deposition rates $\dot{E}_{\rm dep}=120\times10^{51} {\rm ergs s^{-1}}$ and $1.5\times10^{51} {\rm ergs s^{-1}}$. We also find that the peculiar abundance pattern of a Si-deficient metal-poor star HE 1424--0241 can be reproduced by the angle-delimited yield for $\theta=30^\circ-35^\circ$ of the model with $\dot{E}_{\rm dep}=120\times10^{51} {\rm ergs s^{-1}}$.