Radiative accelerations have been calculated in detail for iron in main-sequence models with T eff =6700, 8000, and 10,000 K and log g=4.0 and 4.3 and a number of Fe abundances. Atomic data for Fe IX to Fe XVII were taken from the Opacity Project, and this allowed us to calculate the accelerations over an important fraction of the envelope and to calibrate formulae that were obtained earlier using data from the first few states of ionization. We have derived approximate formulas that allow our results to be used in stellar evolution calculations. From a comparison of radiative acceleration and gravity, one may conclude that only small Fe abundance anomalies are to be expected in those stars with T eff =6700 K where atomic diffusion is important