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The interpretation of total line intensities from optically thin gases

III. Application to coronal forbidden line spectra

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Abstract

The diagnostic method developed in the two preceding papers of this series is applied to coronal forbidden line intensity data obtained at eclipses in 1952, 1961, 1965, 1966, and 1970. The application of the method is limited by the nature of the data but allows a first inference of the relationship between electron density and temperature in the condensations observed at these eclipses, and of the distribution of the electrons within the temperature range samples by the observations effectively 106 to 2.4 × 106 K. We determine the relative abundance of nickel to iron in the corona, finding a value in agreement with latest photospheric determinations and with a similar (factor of two) uncertainty. We are also able to set lower limits to the abundance of iron with respect to hydrogen, again finding values consistent with recent photospheric determinations.

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Authors and Affiliations

  1. Joint Institute for Laboratory Astrophysics, Boulder, Colorado, U.S.A.

    J. T. Jefferies

  2. High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colorado, U.S.A.

    F. Q. Orrall

  3. Institute for Astronomy, University of Hawaii, Honolulu, Hawaii, U.S.A.

    J. B. Zirker

Authors
  1. J. T. Jefferies
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  2. F. Q. Orrall
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  3. J. B. Zirker
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Additional information

Presently on leave of absence from the Institute for Astronomy, University of Hawaii.

Of the National Bureau of Standards and the University of Colorado.

John Simon Guggenheim Memorial Fellow, 1970.

The National Center for Atmospheric Research is sponsored by the National Science Foundation.

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Jefferies, J.T., Orrall, F.Q. & Zirker, J.B. The interpretation of total line intensities from optically thin gases. Sol Phys 22, 327–343 (1972). https://doi.org/10.1007/BF00148700

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  • DOI: https://doi.org/10.1007/BF00148700

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