Two recommendations are made that can eliminate persistent confusion in the study of diatomic spectroscopy by providing uniform and consistent definitions of the electronic transition moments and the rotational line intensity factors. First, it is recommended that the equation for the line strength of asingle rotational line be adopted to specify the relationship between the electronic transition moment and the rotational line intensity factor. Second, it is recommended that the electronic transition moment operator for perpendicular transitions be defined by (1/2]")( Jo, + iby). The adoption of these conventions results in a value of (2s + 1)(2J + 1) for the sum rule of the rotational line intensity factor for 2% * P+ transitions and a value of 2(2S + 1)(2J + 1) for the sum rule for all other spin-allowed transitions.

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Fra nck-Condon factor a rrays h a ve been computed numerica ll y to hi gh vibrationa l qua ntum numbers for t he band syste msB31I -A3~ A32; -X l~ al lI -Xl~

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.