The Photospheric-to-Coronal Iron Abundance from X-ray Lines Observed by YOHKOH and Other Satellites

Details The Photospheric-to-Coronal Iron Abundance from X-ray Lines Observed by YOHKOH and Other Satellites The Photospheric-to-Coronal Iron Abundance from X-ray Lines Observed by YOHKOH and Other Satellites

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994kofu.symp..301p&link_type=abstract

In: Proceedings of Kofu Symposium, Kofu, Japan, Sept. 6-10, 1993, p.301-304.

Physics

1

Scientific paper

We have analyzed the intensities of photospherically formed K_alpha lines (1.936, 1.940A) and the Fe xxv resonance line (1.850A) observed by X-ray spectrometers on the P78-1 and S.M.M. spacecraft to deduce that the photospheric abundance of iron is not significantly different from the coronal abundance, despite recent suggestions that the coronal abundance is up to a factor of about three higher. This result confirms an earlier analysis of yohkoh data using the K_beta line and Fe xxv resonance line features.

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