📝 SummarXiv

Abstract

In the near ultraviolet (NUV) part of the solar spectrum, there are several Fe I lines with very broad profiles, typical of chromospheric lines. These lines are largely unexplored due to the lack of high-resolution data in this region. This changed with the successful Sunrise III flight in 2024, when spectro-polarimetric data were recorded with high spatial, spectral, and temporal resolution covering a large variety of solar targets. The aim of this work is to investigate the formation of the lines and lay the groundwork for further studies. We compute the spectrum of the lines at 358.12 nm, 371.99 nm, 406.36 nm, and 407.17 nm emerging from the standard 1D FAL-atmospheres using the non-local thermodynamic equilibrium (NLTE) radiative transfer code RH. We find that the lines are affected by overionization in the wings, but have line cores strongly affected by scattering. The line cores form well into the chromosphere in the tested atmosphere models except the colder FALX model where the line core forms in the temperature minimum (which lies at traditional chromospheric heights). In the presence of a vertical magnetic field, the Stokes $V$ signal is multi-lobed. The profile can be decomposed into two broad photospheric lobes and two sharper lobes forming in the flanks of the chromospheric line core. We have investigated the properties of four lines of Fe I that form in the lower chromosphere. The results provide a basic understanding of the formation of the lines, which will be useful for later analysis of formation in 3D magnetohydrodynamic simulations and an eventual investigation into their diagnostic potential.