Iron K beta line emission in solar flares observed by YOHKOH and the solar abundance of iron

Details Iron K beta line emission in solar flares observed by YOHKOH and the solar abundance of iron Iron K beta line emission in solar flares observed by YOHKOH and the solar abundance of iron

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...435..888p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 435, no. 2, p. 888-897

Astronomy and Astrophysics

Astrophysics

23

Abundance, Iron, K Lines, Solar Flares, X Ray Spectra, Photosphere, Scientific Satellites, Solar Corona, Statistical Distributions

Scientific paper

A weak line at 1.757 A in solar flare X-ray spectra from the Bragg Crystal Spectrometer (BCS) on Yohkoh is identified as the K beta or inner-shell 1s-3p transition in photospheric iron. The observed line intensity and light curve during several flares suggest that, as with the iron K alpha lines at 1.936 and 1.940 A, excitation occurs principally by fluorescence, with X-ray emission from the hot flare plasma in the low corona exciting photospheric iron atoms. The intensity ratio of the K beta line to the Fe XXV resonance line, which is near in wavelength (1.851 A) and simultaneously observed by the BCS, depends on the photospheric and coronal Fe/H abundance ratio as well as on heliocentric distance and height of the X-ray source. These observations indicate that the coronal Fe/H abundance ratio is not more than a factor of 2 higher than the photospheric. Significant variations from flare to flare cannot be confirmed.

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