A spectral analysis of solar images in the range 180-210 angstrom with theRES-K spectroheliograph onboard the KORONAS-I satellite

A spectral analysis of the solar and solar-corona images that were obtained with the RES-K spectroheliograph onboard the KORONAS-I satellite over four months of observations was performed. Monochromatic images of the entire s olar disk and regions above the limb have been taken in lines of the wavele ngth range 180-210 Angstrom for the first time. More than 60 such images we re recorded with a high space resolution (more than 20 ") and processed. Th e images clearly reveal plasma structures (active regions, coronal holes, r egions of the quiet Sun, condensations above the limb, etc.) which are char acterized by different flux distributions in the line spectra. We present t he spectrum of an active region that was taken on June 4, 1994, 17:20 UT. T his spectrum exhibits the brightest lines of Fe VIII-XIII, S X-XI, O IV-VI, etc., with the excitation temperature typical of the chromosphere-corona t ransition layer and the lower corona. Based on a preliminary analysis of th e total spectra for 40 different areas on and outside the solar disk, we we re able to compile a catalog of 51 lines. The relative intensities of sever al lines, in particular, of the Fe XII triplet, differ markedly from publis hed calculated intensities, which necessitates constructing new models by u sing refined atomic data. The presence of the 192.0 Angstrom line in the re corded spectra, which was tentatively identified with a transition in Fe XX IV, suggests that there is plasma with a temperature of 2 x 10(7) K in acti ve regions in the absence of flares.