Nature . ition to de-termine the relation of this new gas to other gases, bothknown and unknown, appearing in stars of nearly equaltemperature. Other Neiv Gas Lines. But even with our present knowledge of stellar spectrawe find that in relation to the hottest stars there are stillsome gaps in our chemical knowledge : not only is thisso, but have we any right to assume, taking into accountthe limitations of our means of observation and of thestrict limitation of our observations to the relativelysmall part of space nearest us, enormous though it is,that we are as yet really in touch with the hi
Nature . ition to de-termine the relation of this new gas to other gases, bothknown and unknown, appearing in stars of nearly equaltemperature. Other Neiv Gas Lines. But even with our present knowledge of stellar spectrawe find that in relation to the hottest stars there are stillsome gaps in our chemical knowledge : not only is thisso, but have we any right to assume, taking into accountthe limitations of our means of observation and of thestrict limitation of our observations to the relativelysmall part of space nearest us, enormous though it is,that we are as yet really in touch with the highest stellartemperatures ? Again, we cannot be certain that the small number ofstars as yet studied puts us in presence of the higheststellar temperatures. Those stars which apparently areat the very apex of the temperature curve are involvedin unknown lines, and require a special study. Two typical unknown lines have wave-lengths at COMPARISON OF ENHANCCD LINES WITHCHROMOSPHERE AND « CYCNI CHROMOSPHERE. in hydrogen at atmospheric pressure the ordinary seriesof hydrogen lines is very broad. The use of the sparkwith large jars in vacuum tubes results in the partialfusion of the glass and the appearance of lines whichhave been traced to silicium, but the new series hasnot yet been observed. In his first communication. Prof. Pickering mentionslines at 4698, 4652, 4620, and 4505, but he does not referto them in his second paper, which has special referenceto the new series. The line 4505 was at first taken to beone of the components of the new series, but this seemsto have been subsc(|uently superseded by the employ-ment of the line about 4544, which agrees better both asregards intensity and the calculated position 45436. As this new hydrogen series seems to bear the samerelation to the well-known one as the proto-metallic linesbear to the metallic, I call the gas which produces itproto-hydrogen for the sake of clearness. The new series of lines discovered by Prof. Pickeringhas
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