Spectrum Analysis in Its Application to Terrestrial Substances, and the Physical Constitution of the Heavenly Bodies: Familiarly Explained by Dr. H. Schellen, Tr. from the 2d Enl. and Rev. German Edition by Jane and Caroline Lassell

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Longmans, 1872 - 662 pages


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Page 203 - mechanical explanation thus suggested, being particularly opaque for light of that quality, prevents such of it as is emitted from the sun from penetrating to any considerable distance through the surrounding atmosphere. The test of this theory must be had in ascertaining whether or not vapour of sodium has the special absorbing power anticipated.
Page 145 - some compound, probably the oxide of the difficultly reducible metal ; whereas at the enormously high temperature of the intense electric spark these compounds are split up, and thus the true spectrum of the metal is obtained. In none of the spectra of the more reducible alkaline metals (potassium, sodium, lithium) can any deviation or disappearance of
Page 355 - our atmosphere near the sun's edge would be greatly reduced in intensity by the dispersion of the prisms, while the bright lines of the prominences, if such be present, would remain but little diminished in brilliancy. This principle has been carried out by various forms of prismatic apparatus, and also by other contrivances, but hitherto without success."]
Page 203 - of refrangibility of the double line D. Hence the presence of sodium in a source of light must tend to originate light of that quality. On the other hand, vapour of sodium in an atmosphere round a source must have a great tendency to retain
Page 355 - of the red prominences seen during a solar eclipse. The invisibility of these objects at ordinary times is supposed to arise from the illumination of our atmosphere. If these bodies are gaseous, their spectra would consist of bright lines. With a powerful spectroscope the light
Page 389 - • May not the spectroscope afford us evidence of the existence of the ' red flames ' which total eclipses have revealed to us in the sun's atmosphere ; although they escape all other methods of observation at other times
Page 404 - As a rule, the attachment to the chromosphere is narrow, and is not often single; higher up, the stems, so to speak, intertwine, and the prominence expands and soars upward until it is lost in delicate filaments, which are carried away in floating masses.
Page 202 - Stokes mentioned to me at Cambridge some time ago, probably about ten years, that Prof. Miller had made an experiment testing to a very high degree of accuracy the agreement of the double dark line D of the solar spectrum with the double bright line constituting the spectrum of the
Page 473 - The spectra of such stars appear like a row of columns illuminated from the side, producing a stereoscopic effect ; and when the bright bands are narrower than the dark ones, the spectrum has the appearance of a series of grooves. Red stars of even the eighth magnitude have been examined spectroscopically with Secchi's admirable instrument and
Page 356 - I have this morning perfectly succeeded in obtaining and observing part of the spectrum of a solar prominence. As a result I have established the existence of three bright lines in the following positions

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