Observational constraints on the origin of the elements II. 3D non-LTE formation of Ba ii lines in the solar atmosphere

TL;DR

This paper advances solar and stellar abundance modeling by updating 3D non-LTE radiative transfer codes and applying them to determine a precise solar barium abundance, incorporating new atomic data and line effects.

Contribution

It introduces improvements to 3D non-LTE radiative transfer codes and applies them to accurately measure the solar barium abundance using new atomic data.

Findings

First full 3D non-LTE barium abundance of 2.27±0.02±0.01

Inclusion of new atomic data and line effects improves abundance accuracy

Consistent analysis of four Ba II lines in the solar spectrum

Abstract

Context. The pursuit of more realistic spectroscopic modelling and consistent abundances has led us to begin a new series of papers designed to improve current solar and stellar abundances of various atomic species. To achieve this, we have began updating the three-dimensional (3D) non-local thermodynamic equilibrium (non-LTE) radiative transfer code, Multi3D, and the equivalent one-dimensional (1D) non-LTE radiative transfer code, MULTI. Aims. We examine our improvements to these codes by redetermining the solar barium abundance. Barium was chosen for this test as it is an important diagnostic element of the s-process in the context of galactic chemical evolution. New Ba II + H collisional data for excitation and charge exchange reactions computed from first principles had recently become available and were included in the model atom. The atom also includes the effects of isotopic line shifts and hyperfine splitting. Method. A grid of 1D LTE barium lines were constructed with MULTI and fit to the four Ba II lines available to us in the optical region of the solar spectrum. Abundance corrections were then determined in 1D non-LTE, 3D LTE, and 3D non-LTE. A new 3D non-LTE solar barium abundance was computed from these corrections. Results. We present for the first time the full 3D non-LTE barium abundance of $A({\rm Ba})=2.27\pm0.02\pm0.01$, which was derived from four individual fully consistent barium lines. Errors here represent the systematic and random errors, respectively.