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Coronagraphic observations of an enhanced coronal region

II. Temperature and density structure through the enhanced region

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Abstract

Ratios of emission line intensities are used to calculate the variation of temperature and the variation of electron density as a function of ion class for differing paths through a coronal enhancement. The data indicate (a) a peak mean electron density of 2.3 × 109 cm−3, (b) a temperature maximum greater than 2.3 × 106 K, and (c) the non-coincidence of the peak temperature and peak mean electron density. The latter demonstrates the invalidity of the assumption of symmetric models for coronal enhancements.

The abundance of Ni was found to be equal to 0.045 that of Fe from the line ratio I(λ 6702)/ /I(λ 7059) and a density model based on the variation of the ratio I(λ 8024)/I(λ 6702).

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Author notes

  1. Richard R. Fisher

    Present address: Sacramento Peak Observatory, Sunspot, N.M., U.S.A.

Authors and Affiliations

  1. Mees Solar Observatory, Institute for Astronomy, University of Hawaii, H.I., U.S.A.

    Richard R. Fisher

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  1. Richard R. Fisher
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Fisher, R.R. Coronagraphic observations of an enhanced coronal region. Sol Phys 24, 385–394 (1972). https://doi.org/10.1007/BF00153380

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  • DOI: https://doi.org/10.1007/BF00153380

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