# The elemental composition of the Sun III. The neutron capture elements Cu to Th

**Authors:** Nicolas Grevesse, Pat Scott, Martin Asplund, A. Jacques Sauval  
**arXiv:** [1405.0288](https://arxiv.org/abs/1405.0288)  
**Date:** 2014-05-01  
**Summary page:** https://www.summarizepaper.com/en/paper/1405.0288v1/

## Key points

- The paper re-evaluates the abundances of elements in the Sun from copper to thorium.
- Results are based on neutral and singly-ionized lines in the solar spectrum and use the latest 3D hydrodynamic solar model atmosphere.
- Authors correct for departures from local thermodynamic equilibrium (NLTE).
- Stringent line selections, high-quality observational data, and careful assessment of oscillator strengths, hyperfine constants, and isotopic separations available in literature were employed to minimize statistical and systematic uncertainties.
- Results are typically in good agreement with the abundances found in pristine meteorites but reveal some interesting exceptions.
- Analysis constitutes both a full exposition and a slight update of relevant parts of their preliminary results presented in Asplund et al.'s paper (arXiv:0909.0948), including full line lists and details of all input data employed.
- Study provides valuable insights into our understanding of the chemical composition of our nearest star and its implications for our understanding of stellar evolution and nucleosynthesis processes.

## Summary

In their paper "The elemental composition of the Sun III. The neutron capture elements Cu to Th," Nicolas Grevesse, Pat Scott, Martin Asplund, and A. Jacques Sauval re-evaluate the abundances of elements in the Sun from copper ($Z=29$) to thorium ($Z=90$). Their results are based on neutral and singly-ionized lines in the solar spectrum and use the latest 3D hydrodynamic solar model atmosphere. In some cases, they also correct for departures from local thermodynamic equilibrium (NLTE). To minimize statistical and systematic uncertainties, the authors make stringent line selections, employ high-quality observational data, and carefully assess oscillator strengths, hyperfine constants, and isotopic separations available in the literature for every line included in their analysis. The authors' results are typically in good agreement with the abundances found in pristine meteorites but reveal some interesting exceptions. This analysis constitutes both a full exposition and a slight update of relevant parts of their preliminary results presented in Asplund et al. 's paper (arXiv:0909.0948), including full line lists and details of all input data employed. Overall, this study provides valuable insights into our understanding of the chemical composition of our nearest star and its implications for our understanding of stellar evolution and nucleosynthesis processes.