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Non-local thermodynamical equilibrium (non-LTE) line formation for neutraland singly-ionized iron is considered through a range of spectral types whenthe effective temperature varies from 6500 K up to 8500 K, the gravity from logg = 4 down to log g = 3, and the metallicity is solar one. The non-LTEcalculations were performed with a comprehensive model atom for iron which wastreated in our earlier paper (Mashonkina et al. 2011, A&A, 528, A87). Thedepartures from LTE lead to systematically depleted total absorption in the FeI lines and positive abundance corrections, in qualitative agreement with theRentzsch-Holm (1996, A&A, 312, 966) study. However, our predicted magnitude ofthe non-LTE effects is significantly smaller compared to the previous resultsdue to the use of rather complete model atom of Fe I. The non-LTE abundancecorrections do not exceed 0.1 dex for the dwarf models and 0.20 dex for thegiant ones. Non-LTE leads to strengthening the Fe II lines, however, the effectis small, such that the abundance correction is at the level of -0.01 to -0.03dex over the whole range of stellar parameters being considered. No firmconclusion can be drawn with respect to whether or not the Fe I/Fe IIionization equilibrium is fulfilled in the atmosphere of the Sun and Procyondue to uncertainty in available gf-values for visible lines of Fe I and Fe II.

Non-LTE line formation for Fe I and Fe II in the atmospheres of A-F type stars