Fe-peak element abundances in disk and halo stars

TL;DR

This study critically reevaluates iron-peak element abundances in disk and halo stars to address discrepancies in Galactic chemical evolution models and improve understanding of supernova nucleosynthesis.

Contribution

It provides a detailed reassessment of elemental abundance trends, highlighting potential issues in current models and spectroscopic measurements.

Findings

Identifies inconsistencies in observed Fe-peak element trends

Suggests possible deficiencies in stellar yield models

Highlights need for revised spectroscopic abundance determinations

Abstract

At present none of Galactic chemical evolution (GCE) models provides a self-consistent description of observed trends for all iron-peak elements with metallicity simultaneously. The question is whether the discrepancy is due to deficiencies of GCE models, such as stellar yields, or due to erroneous spectroscopically-determined abundances of these elements in metal-poor stars. The present work aims at a critical reevaluation of the abundance trends for several odd and even-Z Fe-peak elements, which are important for understanding explosive nucleosynthesis in supernovae.