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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.

A sequence of thirty-five ultraviolet photographic spectra of the Sun has been obtained in the wavelength region 850-2190 Â, as a function of time during the eclipse. These cover the range from before second contact until midtotality, with a spatial resolution of the order 2 arc sec. A general description of the experiment and data is given. Twenty-five new coronal lines have been seen, the majority of which have been identified as new forbidden transitions. The La corona is observed out to over 1.5 Rq, and a quantitative interpretation is presented. Analyses of other features-e.g., prominences, quiet-atmosphere structure, and coronal condensations-are continuing.

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