We present a measurement of the abundance of Fe relative to H in the solar corona using a technique which differs from previous spectroscopic and solar wind measurements .
Our method combines EUV line data from the CDS spectrometer on SOHO with thermal bremsstrahlung radio data from the VLA .
The coronal Fe abundance is derived by equating the thermal bremsstrahlung radio emission calculated from the EUV Fe line data to that observed with the VLA , treating the Fe/H abundance as the sole unknown .
We apply this technique to a compact cool active region and find Fe/H = 1.56 \times 10 ^ { -4 } , or about 4 times its value in the solar photosphere .
Uncertainties in the CDS radiometric calibration , the VLA intensity measurements , the atomic parameters , and the assumptions made in the spectral analysis yield net uncertainties \sim 20 % .
This result implies that low first ionization potential elements such as Fe are enhanced in the solar corona relative to photospheric values .