Kinetic equilibrium of iron in the atmospheres of cool dwarf stars - II. Weak FeI lines in the solar spectrum

NLTE line formation calculations of Fe I in the solar atmosphere are extend ed to include weak lines in the visual spectrum of the Sun. Previously esta blished atomic models are used to discriminate between different ways of tr eating collisional interaction processes. As indicated by the analysis of s trong Fe I lines, the influence of deviations from LTE in the solar atmosph ere on the Fe abundance is small for all lines. To derive a common solar Fe I abundance from both strong and weak lines fine-tuning of the microturbul ence velocity parameter and the van der Waals damping constants is required . The solar Fe I abundances based on all available f-values are dominated b y the large scatter already found for the stronger lines. In particular the bulk of the data from the work of May et al. and O'Brian et al. is not ade quate for accurate abundance work. Based on f-values measured by the Hannov er and Oxford groups alone, the Fe I LTE abundances are log epsilon (Fe I, circle dot) = 7.57 for the empirical and log epsilon (Fe I, circle dot) = 7 .48...7.51 for the line-blanketed solar model. The solar Fe ionization equi librium obtained for different atomic and atmospheric models rules out NLTE atomic models with a low efficiency of hydrogen collisions. At variance wi th Paper I, it is now in better agreement with laboratory Fe ii f-values fo r all types of line-blanketed models. Our final model assumptions consisten t with a single unique solar Fe abundance log epsilon (Fe, circle dot) simi lar to 7.48...7.51 calculated from NLTE line formation are (a) a line-blank eted solar model atmosphere, (b) an iron model atom with hydrogen collision rates 0.5 < S-H < 5 times the standard value to compensate for the large p hotoionization cross-sections, (c) a microturbulence velocity xi (t) = 1.0 km s(-1), (d) van der Waals damping parameters decreased by Delta log C-6 = -0.10...0.15 as compared to Anstee & O'Mara's calculations, depending on S -H, (e)Fe II f-values as published by Schnabel et al., and (f) Fe I f-value s published by the Hannover and Oxford groups.