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