Abstract
IN the third article under the above heading, when referring to the suggested programme for the observations of the next eclipse, I stated briefly the divergent views held with regard to the true locus of origin of the absorption which produces the Fraunhofer lines. It is, I think, worth while to return to this subject in order that the results obtained from the double series of photographs obtained during the eclipse of 1893 may be indicated. I pointed out that in the photographs in question the radiation spectrum was most distinctly not identical with the Fraunhofer spectrum; the most important point being that some of the strongest bright lines do not appear among the dark ones in the solar spectrum, while some of the strongest dark lines are not seen bright in the spectrum of the stratum of vapours in immediate contact with the photosphere. The region covered by the diagram, given in my paper in the Phil. Trans., lies between wave-lengths 4100 and 4300, but similar results follow when other regions are included in the inquiry.
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References
Phil Trans., 1893, vol. clxxxiv. A. p. 684.
"Astronomy and Astrophysics," 1892, pp. 50, 602, 618.
Roy. Soc. Proc., 1879, vol. xxviii. p. 13.
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LOCKYER, N. The Approaching Total Eclipse of the Sun1: VI. Nature 56, 445–449 (1897). https://doi.org/10.1038/056445b0
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DOI: https://doi.org/10.1038/056445b0