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Solar abundance determination from ultraviolet emission lines

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Abstract

The intensities of far ultraviolet emission lines from the solar corona are analyzed to determine relative coronal abundances for oxygen, silicon, and iron. Dielectronic recombination is included in the formulation of ionization equilibrium. Observations of solar radio emission are used to obtain abundances relative to hydrogen. The absolute coronal abundances appear to be in agreement with their respective photospheric values. General properties of the structure of the chromosphere and corona are deduced from the analysis of observed emission in the ultraviolet and radio wavelength regions.

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Authors and Affiliations

  1. Harvard College Observatory, Cambridge, Mass., U.S.A.

    Andrea K. Dupree & Leo Goldberg

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  1. Andrea K. Dupree
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  2. Leo Goldberg
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Dupree, A.K., Goldberg, L. Solar abundance determination from ultraviolet emission lines. Sol Phys 1, 229–241 (1967). https://doi.org/10.1007/BF00150858

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  • DOI: https://doi.org/10.1007/BF00150858

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