Abstract
The abundance of Fe relative to H is obtained by using resonantly scattered intensities of λ 284 of Fe XV that were measured with OSO-7 and resonantly scattered intensities of Lα of H I that were obtained by Gabriel (1971). Because of possible differences in electron densities along lines of sight for these non-simultaneous measurements and in relative calibrations, results are rather uncertain but still indicate that the average Fe abundance relative to H in the corona appears to be at least as large as a recent photospheric abundance. Some limitations in using this method for obtaining abundances are examined for future experiments with simultaneous measurements and well calibrated detectors.
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Nakada, M.P., Chapman, R.D., Neupert, W.M. et al. Abundance of Fe relative to H at 1.5 solar radii. Sol Phys 42, 487–496 (1975). https://doi.org/10.1007/BF00149928
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DOI: https://doi.org/10.1007/BF00149928