Accurate abundance analysis of late-type stars: advances in atomic physics

TL;DR

This paper reviews recent advances in atomic physics that improve the accuracy of chemical abundance measurements in late-type stars, integrating theoretical, experimental, and astrophysical modeling efforts.

Contribution

It provides a comprehensive overview of atomic data and processes crucial for high-precision stellar abundance analysis, highlighting recent progress and interdisciplinary integration.

Findings

Enhanced atomic data accuracy improves stellar abundance measurements.

Integration of laboratory measurements and theoretical models advances spectral analysis.

Progress supports more precise determination of stellar properties.

Abstract

The measurement of stellar properties such as chemical compositions, masses and ages, through stellar spectra, is a fundamental problem in astrophysics. Progress in the understanding, calculation and measurement of atomic properties and processes relevant to the high-accuracy analysis of F-, G-, and K-type stellar spectra is reviewed, with particular emphasis on abundance analysis. This includes fundamental atomic data such as energy levels, wavelengths, and transition probabilities, as well as processes of photoionisation, collisional broadening and inelastic collisions. A recurring theme throughout the review is the interplay between theoretical atomic physics, laboratory measurements, and astrophysical modelling, all of which contribute to our understanding of atoms and atomic processes, as well as to modelling stellar spectra.