Radiative transfer in stellar atmospheres

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The chemical make-up of the Sun: A 2020 vision (2021, unknown): “These abundance analyses have mostly been within the framework of local thermodynamic equilibrium (LTE), thus assuming the Boltzmann, Saha, and Guldberg-Waage distributions for the atomic and molecular level populations and the Planck function for the radiation source function (e.g., Rutten 2003).”
Non-LTE line formation of Fe in late-type stars - II. 1D spectroscopic stellar parameters (2012, background): “We take the term overionisation to imply thatniPi j − n jP ji > 0, whereni is the level population of a bound state of Fe I, andn j is the ground state of Fe II (notations follow Rutten 2003).”
Recent variability of the solar spectral irradiance and its impact on climate modelling (2012, background): “2.6 of Rutten, 2003) in the solar atmosphere, as well1015 as by the temporal and spatial bifurcations of the temperature and density in the solar atmosphere (Carlsson and Stein, 1997; Uitenbroek and Criscuoli, 2011).”