Signs of atmospheric inhomogeneities in cool stars from 1D-NLTE analysis of iron lines

TL;DR

This study investigates atmospheric inhomogeneities in cool stars by analyzing iron lines using 1D-NLTE models, revealing discrepancies with 3D-LTE predictions and assessing the applicability of <3D> models for different lines and conditions.

Contribution

It provides a detailed comparison of 1D-NLTE and 3D-LTE line formation models for iron in cool stars, highlighting limitations and conditions for their validity.

Findings

Discrepancies between observed and predicted Fe I line abundances.

NLTE abundances from Fe I and Fe II agree when low-excitation lines are ignored.

<3D> models are only suitable for specific lines and physical conditions.

Abstract

For the well studied halo star HD 122563 and the four stars in the globular cluster NGC 6397, we determine NLTE abundances of iron using classical plane-parallel model atmospheres. Each star reveals a discrepancy in abundances between the Fe I lines arising from the ground state and the other Fe I lines, in qualitative agreement with the 3D-LTE line formation predictions, however, the magnitude of the observed effect is a factor of 2 smaller compared with the predicted one. When ignoring the Fe I low-excitation lines, the NLTE abundances from the two ionization stages, Fe I and Fe II, are consistent in each investigated star. For the subgiants in NGC 6397, this is only true when using the cooler effective temperature scale of Alonso et al. (1999). We also present full 3D-LTE line formation calculations for some selected iron lines in the solar and metal-poor 4480/2/-3 models and NLTE calculations with the corresponding spatial and temporal average <3D> models. The use of the <3D> models is justified only for particular Fe I lines in particular physical conditions. Our NLTE calculations reproduce well the centre-to-limb variation of the solar Fe I 7780 A line, but they are unsuccessful for Fe I 6151 A. The metal-poor <3D> model was found to be adequite for the strong Fe I 5166 A (Eexc = 0) line, but inadequite in all other investigated cases.