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

Details A spectral analysis of solar images in the range 180-210 Å with the RES-K spectroheliograph onboard the KORONAS-I satellite A spectral analysis of solar images in the range 180-210 Å with the RES-K spectroheliograph onboard the KORONAS-I satellite

Nov 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998astl...24..819z&link_type=abstract

Astronomy Letters, Volume 24, Issue 6, November 1998, pp.819-825; Pis'ma v Astronomicheskii Zhurnal, Vol. 24, p. 943

Astronomy and Astrophysics

Astronomy

7

Scientific paper

A spectral analysis of the solar and solar-corona images that were obtained with the RES-K spectro-heliograph onboard the KORONAS-I satellite over four months of observations was performed. Monochromatic images of the entire solar disk and regions above the limb have been taken in lines of the wavelength range 180-210 Angstroms for the first time. More than 60 such images were recorded with a high space resolution (more than 20'') and processed. The images clearly reveal plasma structures (active regions, coronal holes, regions of the quiet Sun, condensations above the limb, etc.) which are characterized by different flux distributions in the line spectra. We present the spectrum of an active region that was taken on June 4, 1994, 17:20 UT. This 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 transition layer and the lower corona. Based on a preliminary analysis of the total spectra for 40 different areas on and outside the solar disk, we were able to compile a catalog of 51 lines. The relative intensities of several lines, in particular, of the Fe XII triplet, differ markedly from published calculated intensities, which necessitates constructing new models by using refined atomic data. The presence of the 192.0 Anstroms line in the recorded spectra, which was tentatively identified with a transition in Fe XXIV, suggests that there is plasma with a temperature of 2 x 10^7 K in active regions in the absence of flares.

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