Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995adspr..15q..33p&link_type=abstract
Advances in Space Research (ISSN 0273-1177), vol. 15, no. 7, p. (7)33-(7)36
Astronomy and Astrophysics
Astronomy
4
Abundance, Iron, K Lines, Photosphere, Solar Corona, Solar X-Rays, Stellar Models, X Ray Astronomy, X Ray Spectra, Hydrogen, Solar Flares, Solar Maximum Mission, Solar Spectrometers, Solar Temperature, X Ray Fluorescence
Scientific paper
The Fe K-alpha and K-beta X-ray lines (wavelengths 1.94 and 1.76 A) in the solar X-ray spectrum are formed by fluorescence of photospheric iron atoms, and the ratio of the intensity of either to the He-like iron (Fe XXV) resonance line at 1.85 A is a function of the photospheric-to-coronal abundance of iron. The temperature dependence of this ratio is weak as long as the flare temperature Te greater than or approximately equal to 15 x 106K. Comparison of the theoretical value of this intensity ratio with observations from crystal spectrometers on Yohkoh, Solar Maximum Mission (SMM) and P78-1 are consistent with the photospheric abundance of Fe being equal to the coronal.
Fludra Andrzej
Lang Jaclyn
Phillips Kenneth J. H.
Pike David C.
Takahashi Minoru
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