Abstract
Theoretical line intensity ratios involving Fe xii transitions in the 186–201 Å wavelength range are compared with observational data for five solar active regions, obtained by the RES-C spectroheliograph on the CORONAS-I mission. Generally good agreement is found between theory and observation, hence resolving discrepancies previously found in the comparison of calculations with active region and subflare spectra from the Solar EUV Rocket Telescope and Spectrograph (SERTS). However, the Fe xii 190.06- and 201.12-Å lines are blended with Fe x 190.04 Å and Fe xiii 201.13 Å, respectively. In addition, a weak feature at ∼197 Å, tentatively identified as Fe xii 196.87 Å, does not appear to be due to this ion.
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