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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Common terms and phrases
absorption according amount appear atmosphere bands become blue body bright lines brilliant carbon changes chromosphere coincident colour comet compared complete consists contains continuous corona dark lines direction disk dispersive displacement distance drawing earth eclipse edge electric employed F-line faint flame Fraunhofer lines give given glass greater green halo heat Huggins hydrogen incandescent inches increased intensity Kirchhoff length lens less light Lockyer luminous marked means measured metals miles moon motion nature nebula object observed obtained pass phenomena photographic plate portion position present prism produced prominences rays remarkable represented scale Secchi seen separated shown shows side similar slit sodium solar spectrum space spectra spectroscope spot star substance sufficient sun's sun's limb surface surrounded taken telescope temperature tube vapour various violet visible whole yellow
Popular passages
Page 195 - In the year 1860, he published his memoir on the relation between the emissive and absorptive powers of bodies for heat, as well as for light, in which occurs the celebrated sentence : " The relation between the power of emission and the power of absorption of one and the same class of rays, is the same for all bodies at the same temperature...
Page 568 - ... bands. A fair measure was obtained of the centre of the middle band, which was the brightest ; it gives for this band a wave-length of about 510 millionths of a millimetre. I was not able to do more than estimate roughly the position of the less refrangible band. The result gives 545 millionths. The third band was situated at about the same distance from the middle band on the more refrangible side. It would appear that this comet is similar in constitution to the comets which I examined in 1868*....
Page 371 - With a powerful spectroscope the light reflected from our atmosphere near the sun's limb 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 iii - SCHELLEN'S SPECTRUM ANALYSIS, in its application to Terrestrial Substances and the Physical Constitution of the Heavenly Bodies. Translated by JANE and C. LASSELL; edited, with Notes, by W. HUGGINS, LL.D. FRS With 13 Plates (6 coloured) and 223 Woodcuts. 8vo. price 28s. CELESTIAL OBJECTS for COMMON TELESCOPES.
Page 619 - Kirchhoff's map, determined by direct comparison with the map at the time of observation. In some cases an interrogation mark is appended, which signifies not that the existence of the line is doubtful, but only that its precise place could not be determined, either because it fell in a shading of...
Page 194 - In connexion with this subject it may not be out of place to introduce the following extract of a letter from Prof. W. Thomson to Prof. Kirchhoff, dated 1860. Prof. Thomson thus writes : — ' Professor Stokes mentioned to me at Cambridge some time ago, probably about ten years, that Professor 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...
Page 135 - Bunsen flame or a weak spark, the spectrum observed is produced by 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 maxima of light be noticed on change of temperature.
Page 636 - This paper gives the wave-lengths of the principal lines of the Solar Spectrum. On Wave-lengths. Silliman's Journal, March 1869. GLADSTONE, JH Notes on the Atmospheric Lines of the Solar Spectrum, and on certain Spectra of Gases.
Page 366 - ... as consisting of separate rays, others give to it an almost true geometrical contour; in some of the Spanish sketches a tendency to assume a roughly quadrangular form can be detected, while in most of the Sicilian drawings there is a tendency to an annular form. We pass to the spectroscopic observations of the corona and halo. Prof. Winlock, using a spectroscope of two prisms on a five and a half inch achromatic, found a faint continuous spectrum. Of the bright lines, the most persistent was...
Page 621 - I would call especial attention to the lines numbered 1 and 82 in the catalogue; they are very persistently present, though faint, and can be distinctly seen in the spectroscope to belong to the chromosphere as such, not being due, like most of the other lines, to the exceptional elevation of matter to heights where it does not properly belong. It would seem very probable that both these lines are due to the same substance which causes the DJ line.
Bibliographic information
| Title | 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 |
| Author | Heinrich Schellen |
| Editor | Sir William Huggins |
| Translated by | Caroline Lassell, Jane Lassell |
| Publisher | Longmans, 1872 |
| Original from | the New York Public Library |
| Digitized | 20 Apr 2006 |
| Length | 662 pages |
| Export Citation | BiBTeX EndNote RefMan |