SMM observations of K-alpha radiation from fluorescence of photospheric iron by solar flare X-rays

Details SMM observations of K-alpha radiation from fluorescence of photospheric iron by solar flare X-rays SMM observations of K-alpha radiation from fluorescence of photospheric iron by solar flare X-rays

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...279..866p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 279, April 15, 1984, p. 866-874. Research supported by the Science and Engi

Astronomy and Astrophysics

Astrophysics

24

K Lines, Solar Flares, Solar X-Rays, X Ray Spectra, Iron, Monte Carlo Method, Photosphere, Solar Maximum Mission, Solar Spectra

Scientific paper

High-resolution Fe K-alpha spectra near 1.94 A observed during solar flares with the Bent Crystal Spectrometer on the Solar Maximum Mission are presented. The evidence for two possible excitation mechanisms, electron impact and fluorescence, is examined. It is found that the fluorescence mechanism satisfactorily describes the results, while the observations do not support electron collisional excitation of the Fe K-alpha transitions in low ionization stages (II-XII) of iron. Using Bai's model of the fluorescent excitation process, the photospheric iron abundance relative to that of hydrogen is estimated to be 5-6 x 10 to the -5th. The mean height of the soft X-ray source producing the K-alpha fluorescence is calculated on the basis of this model for about 40 large flares. The solar K-alpha lines are found to be about 25 percent wider than those measured in the laboratory. Weak line features observed at wavelengths shorter than that of the K-alpha lines are discussed.

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