The Solar Hydrogen Spectrum in Non-Local Thermodynamic Equilibrium

We investigate the synthesis of the Balmer and Paschen lines of the quiet Sun, using both classical semiempirical and theoretical model atmospheres, modern line-broadening theory, and non-LTE line formation. The computations alleviate long-standing discrepancies between LTE predictions and the observed lines. Theoretical and semiempirical model atmospheres without a chromosphere on the one hand and semiempirical models with a chromosphere on the other produce two physically disjoint solutions for the run of non-LTE level populations, including H II, throughout the model stratification. The resulting synthetic non-LTE line profiles are practically identical and reproduce the observation in either case, despite large differences in the line-formation depths, e.g., a chromospheric origin of the Hα core (in concordance with observation) versus a photospheric origin. The findings are of much broader interest, assuming the Sun to be a prototype cool dwarf star. A consistent account for chromospheres in cool star analyses is required, because of their potential to change atmospheric structure via non-LTE effects on the ionization balance of hydrogen and thus the free-electron pool. The latter in turn affects the main opacity source H - . This will in particular affect the atmospheres of metal-poor and evolved stars, in which the contribution of hydrogen to the electron pool becomes dominant.