High-precision stellar abundances of the elements - methods and applications

TL;DR

This paper reviews methods for achieving high-precision stellar element abundances in F, G, and K stars, highlighting their astrophysical implications and future potential for understanding stellar and galactic evolution.

Contribution

It introduces advanced techniques for precise abundance measurements and discusses their applications and challenges in stellar and galactic studies.

Findings

High-precision abundances reveal discrete stellar populations.

Differences in abundance-temperature relations for Sun and twins.

Abundance ratios correlate tightly with stellar age.

Abstract

Methods to determine abundances of the elements in the atmospheres of F, G, and K stars with precisions of 0.01-0.03 dex are reviewed. Such high-precision stellar abundances have led to the discovery of unexpected phenomena and relations with important bearings on the astrophysics of galaxies, stars, and planets, such as existence of discrete stellar populations in the Galactic disk and halo, differences in the relation between abundances and elemental condensation temperature for the Sun and solar twins, differences in chemical composition between binary star components and between members of star clusters, and tight relations between some abundance ratios and age for solar-like stars. We conclude that if high-precision abundances can be achieved in studies of more distant stars and stars on the giant and supergiant branches, many more interesting future applications, of great relevance to stellar and galaxy evolution, will be possible. Hence, in planning abundance surveys, it is important to carefully balance the need for large samples of stars against the spectral resolution and signal-to-noise ratio needed to obtain high-precision abundances. Furthermore, it is an advantage to work differentially on stars with similar atmospheric parameters, because then a simple 1D LTE analysis of stellar spectra may be sufficient. However, when determining high-precision absolute abundances or differential abundances between stars having more widely different parameters, e.g. metal-poor stars compared to the Sun or giants to dwarfs, then 3D non-LTE effects must be taken into account.