Quantitative comparison of opacities calculated using the $R$-matrix and Distorted-Wave methods: Fe XVII

TL;DR

This study compares Fe XVII opacities calculated with $R$-matrix and distorted-wave methods, highlighting the importance of autoionizing levels, broadening effects, and configuration interactions for accurate stellar opacity modeling.

Contribution

It provides a detailed comparison of $R$-matrix and DW calculations for Fe XVII, including new extensive Dirac $R$-matrix data and autoionizing level effects, advancing opacity accuracy.

Findings

$R$-matrix and DW results are consistent with similar treatments.

Autoionizing initial levels significantly affect opacities.

Persistent differences remain between calculations and experimental data.

Abstract

We present here a detailed calculation of opacities for Fe~XVII at the physical conditions corresponding to the base of the Solar convection zone. Many ingredients are involved in the calculation of opacities. We review the impact of each ingredient on the final monochromatic and mean opacities (Rosseland and Planck). The necessary atomic data were calculated with the $R$-matrix and the distorted-wave (DW) methods. We study the effect of broadening, of resolution, of the extent of configuration sets and of configuration interaction to understand the differences between several theoretical predictions as well as the existing large disagreement with measurements. New Dirac $R$-matrix calculations including all configurations up to the $n=$ 4, 5 and $6$ complexes have been performed as well as corresponding Breit--Pauli DW calculations. The DW calculations have been extended to include autoionizing initial levels. A quantitative contrast is made between comparable DW and $R$-matrix models. We have reached self-convergence with $n=6$ $R$-matrix and DW calculations. Populations in autoionizing initial levels contribute significantly to the opacities and should not be neglected. The $R$-matrix and DW results are consistent under the similar treatment of resonance broadening. The comparison with the experiment shows a persistent difference in the continuum while the filling of the windows shows some improvement. The present study defines our path to the next generation of opacities and opacity tables for stellar modeling.