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It has been calculated, from a study of the phenomena noted above, that the bright-line star in beta Lyræ is situated at a distance of about fifteen million miles from the center of gravity of the curiously complicated system of which it forms a part. We have not yet exhausted the wonders of Lyra.
With noteworthy and confident prescience, Lockyer, in 1866, before anything was yet known regarding the constitution of the "red flames," ordered a strongly dispersive spectroscope for the express purpose of viewing, apart from eclipses, the bright-line spectrum which he expected them to give. Various delays, however, supervened, and the instrument was not in his hands until October 16, 1868.
The components of groups, still involved and entangled with "silver braids" of cosmic mist, show, perhaps invariably, spectra of the helium type, occasionally crossed by bright rays. Possibly all such stars have passed through a bright-line stage; but further evidence on the point is needed.
Now the spectroscope offers the means of indefinitely weakening atmospheric glare by diffusing a constant amount of it over an area widened ad libitum. But monochromatic or "bright-line" light is, by its nature, incapable of being so diffused. It can, of course, be deviated by refraction to any extent desired; but it always remains equally concentrated, in whatever direction it may be thrown.
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