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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    Titel :

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


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

    Erschienen in:

    Erscheinungsdatum :

    1995-07-01



    Medientyp :

    Sonstige


    Format :

    Keine Angabe


    Sprache :

    Englisch


    Schlagwörter :



    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




    X-Ray Activity in Coronal Loops and Its Photospheric/Chromospheric Signatures

    Sakurai, T. / Shibata, K. / Ichimoto, K. et al. | British Library Conference Proceedings | 1994