Physics
Scientific paper
May 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976rspta.281..375p&link_type=abstract
(Royal Society, Discussion on the Physics of the Solar Atmosphere, London, England, Jan. 14, 15, 1975.) Royal Society (London),
Physics
Line Spectra, Skylab Program, Solar Spectra, Solar X-Rays, X Ray Spectra, Fine Structure, H Alpha Line, High Resolution, Spectral Resolution, Temperature Effects, X Ray Telescopes
Scientific paper
The paper discusses high-resolution scans of several lines in the solar X-ray spectrum. These include the strong lines of the neon-like ion Fe XVII and the temperature-dependent satellite lines observed on the long-wavelength side of the resonance lines of the helium-like ions O VII, Ne IX, and Mg XI. The identifications and relative intensities of the satellite lines are given, and it is shown that the degree of ionization or recombination of the plasma being studied can be estimated by measuring changes in the intensity of the 2S-2P line relative to the 2P-2D line. An energy-level diagram of Fe XVII is presented along with a high-resolution scan of an active-region spectrum between 13 and 18 A with a KAP crystal. A collaborative experiment is briefly reviewed in which simultaneous X-ray images and spectra were obtained with the X-ray telescope aboard Skylab and a rocket-borne X-ray spectrometer. Based on the results of this experiment, the abundance ratio O:Ne:Mg:Si:Fe is estimated to be 7:1:1:1:1.
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