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 fluoroescence 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 T(sub e) greater than or approximately equal to 15 x 10(exp 6)K. 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.


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    Title :

    Evidence for the equality of the solar photospheric and coronal abundance of iron


    Contributors:
    Phillips, K. J. H. (author) / Pike, C. D. (author) / Lang, J. (author) / Zarro, D. M. (author) / Fludra, A. (author) / Watanabe, T. (author) / Takahashi, M. (author)

    Published in:

    Publication date :

    1995-07-01



    Type of media :

    Miscellaneous


    Type of material :

    No indication


    Language :

    English


    Keywords :



    Evidence for the Equality of the Solar Photospheric and Coronal Abundance of Iron

    Phillips, K. J. H. / Pike, C. D. / Lang, J. et al. | British Library Conference Proceedings | 1995




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