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In the early part of August, 1890, the photographic work of the normal solar spectrum which I had undertaken had been carried as far as great A, or the limit of visibility in the red, and to λ 8350, or beyond z, in the invisible regions. During the two previous months of continuously dull weather, while classifying and comparing results, I was interested, on making a close examination of the head portion of the A line, to find the symmetrical construction, the rhythmical grouping, the harmonic order of sequence, and other characteristics of the B line repeated here in every detail.

On the geometrical construction of the oxygen absorption lines great A, great B, and α of the solar spectrum