Abstract
IN a recently published volume1 I endeavoured to bring together the facts relating not only to the distribution of stars generally, but to those which the spectroscope has more recently brought before us touching the distribution of the various chemical groups of stars. One of the interesting results of the inquiry was that the Milky Way, which dominates the general distribution, is also the region of the heavens in which undoubted nebulæ giving us bright-line spectra most do congregate. Nor is this all. Those so-called “stars,” in the spectra of which bright lines are seen, “bright-line stars” and “new stars,” which I have elsewhere shown are nebulas or stars associated with nebulæ, are also almost entirely confined to the Milky Way. The new spectroscopic knowledge, although so priceless to the-student of the chemistry of space, tells us, however, nothing as to the distances of the bodies from us; it only tells us that they lie in the galactic, plane. If, however, we combine with the chemical facts the results, obtained by Monck, Kapteyn and others touching the proper motions of the various kinds of stars as defined by their spectra, the results we obtain are most definite.
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References
"Inorganic Evolution," pp. 124–143.
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LOCKYER, N. Our Stellar System . Nature 63, 29–32 (1900). https://doi.org/10.1038/063029d0
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DOI: https://doi.org/10.1038/063029d0
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