The ratio of the Fe abundance in the photosphere to that in coronal flare plasmas is determined by X‐ray lines within the complex at 6.7 keV (1.9 Å) emitted during flares. The line complex includes the He‐like Fe (Fe xxv) resonance line w (6.70 keV) and Fe Kα lines (6.39 and 6.40 keV), the latter being primarily formed by the fluorescence of photospheric material by X‐rays from the hot flare plasma. The ratio of the Fe Kα lines to the Fe xxvw depends on the ratio of the photospheric to flare Fe abundance, heliocentric angle θ of the flare and the temperature Te of the flaring plasma. Using high‐resolution spectra from X‐ray spectrometers on the P78‐1 and Solar Maximum Mission spacecraft, the Fe abundance in flares is estimated to be 1.6 ± 0.5 and 2.0 ± 0.3 times the photospheric Fe abundance, the P78‐1 value being preferred as it is more directly determined. This enhancement is consistent with results from X‐ray spectra from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) spacecraft, but is significantly less than a factor of 4 as in previous work.