On the appearance of the cleveite and other new gas lines in the hottest stars
In my recent paper on “The Chemistry of the Hottest Stars,” I left for future discussion the spectra of those stars apparently at or near the apex of the temperature curve, for the reason that in them the lines of known gases do not show very great variations, while the enhanced lines cease to be of service as a criterion of temperature. I pointed out, however, that there were several lines, as yet of unknown origin, which are strong in some of these stars and weaker in others, and that the study of these might eventually help us in classifying such stars and arranging them in temperature order, but that before attempting to use the unknown lines in these inquiries it was important in the first instance to discriminate, if possible, between gaseous and metallic lines. Until this point was investigated the relative behaviour of the lines of hydrogen and cleveite gases near the upper temperature limit could not be satisfactorily discussed.