  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~\AA)
emitted during flares. The line complex includes the He-like Fe (\fexxv)
resonance line $w$ (6.70~keV) and Fe K$\alpha$ lines (6.39, 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 K$\alpha$ lines to the
\fexxv\ $w$ depends on the ratio of the photospheric-to-flare Fe abundance,
heliocentric angle $\theta$ of the flare, and the temperature $T_e$ of the
flaring plasma. Using high-resolution spectra from X-ray spectrometers on the
{\em P78-1} and {\em Solar Maximum Mission} spacecraft, the Fe abundance in
flares is estimated to be $1.6\pm 0.5$ and $2.0 \pm 0.3$ times the photospheric
Fe abundance, the {\em P78-1} value being preferred as it is more directly
determined. This enhancement is consistent with results from X-ray spectra from
the {\em RHESSI} spacecraft, but is significantly less than a factor 4 as in
previous work.
