A Treatise on Astronomical Spectroscopy: Being a Translation of Die Spectralanalyse Der Gestirne by Professor Dr. J. Scheiner ... Tr., Rev. and Enl., with the Coöperation of the Author, by Edwin Brant Frost ....Ginn, 1894 - 482 Seiten |
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A Treatise on Astronomical Spectroscopy J. Scheiner,Edwin Brant Frost Keine Leseprobe verfügbar - 2018 |
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A(wv absorption angle Ångström aperture appear ARC IN SUN atmosphere Aurigae aurora band body bright lines broad broadened chromosphere collimating lens collimator comets component continuous spectrum Cygni cylindric lens dark lines deviation dispersion displacement distance E IIIa edge employed eyepiece Fe Fe Fe focal length focal plane Fraunhofer lines gases Geissler tube grating Huggins hydrocarbon hydrogen lines IIIa IIIa IIIb incandescent intensity Jour light line of sight luminous measurements micrometer motion nebulae Nova Aurigae objective objective-prism observing telescope obtained Orionis Phil photographic photosphere Phys planetary nebulae plate Pogg portion Potsdam prism Proc prominence rays refracting refrangible rotation Rowland's Schj screw sity ance slit solar lines solar spectrum SPECTRAL CLASS spectral lines spectre solaire spectroscope spectroscopic observations star's stars of Class stellar spectra surface temperature tenth-meters tube Ueber ultra-red vapor velocity violet visible Vogel WAVE wave-lengths zodiacal light
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Seite 471 - Mathematical and Physical Papers. By GEORGE GABRIEL STOKES, MA, DCL, LL.D., FRS, Fellow of Pembroke College and Lucasian Professor of Mathematics. Reprinted from the Original Journals and Transactions, with additional Notes by the Author. Vol. I. Demy 8vo, cloth, 1jj. Vol.11. In the Press. Mathematical and Physical Papers.
Seite 338 - CAMPBELL, WW: The Reduction of Spectroscopic Observations of Motions in the Line of Sight, Astronomy and Astrophysics, 11, 319, 1892.
Seite 230 - Leyden-jar power ; it may be looked upon therefore as an indication of relatively high temperature. As the line in question has been reversed by one of us in the spectrum of the chromosphere, it follows that the chromosphere, when cool enough to absorb, is still of a relatively high temperature.
Seite 231 - Under certain conditions of temperature and pressure, the very complicated spectrum2 of hydrogen is reduced in our instrument to one line in the green? corresponding to F in the solar spectrum. III. The equally complicated spectrum of nitrogen is similarly reducible to one bright line in the green, with traces of other more refrangible faint lines.
Seite 278 - G of the solar spectrum, glimpses were obtained of a fourth and faint bright line. At the extreme end of the visible part of the less refrangible end of the spectrum, about C, appeared a line brighter than the normal relative brilliancy of this part of the spectrum. The brightness of this line, however, was not nearly so marked in proportion to that of the...
Seite 198 - ... that the telluric lines appear stronger in the less refrangible portions of the spectrum of the planet than in the solar spectrum. There can therefore be no doubt that the atmosphere of Venus exerts an absorption similar to that of our own, and hence the nature of the two atmospheres must be similar We may safely assume that the clouds of Venus consist of condensed aqueous vapor, thus again resembling those of the earth.
Seite 278 - In the telescope it was surrounded with a faint nebulous haze, extending to a considerable distance, and gradually fading away at the boundary.
Seite vi - D's and the reversal and occasional "lumping" of C has been noticeable even with this high dispersion. But the most striking result is that in certain regions the spectrum of the spot-nucleus, instead of appearing as a mere continuous shade, crossed here and there by markings dark and light, is resolved into a countless number of lines, exceedingly fine and closely packed, interrupted frequently between E and F (and occasionally below E) by lines as bright as the spectrum outside the spot.
Seite 247 - Cephei with those like a. Cygni makes it here important to discuss the place of a Cygni in Vogel's classification. With regard to this star Dr. Scheiner writes : " The spectrum of a. Cygni, in spite of the large number of its lines, has no resemblance with that of the sun. While it is possible to identify most of the lines with solar lines in respect of their position, yet the total lack of agreement ns to intensity of the lines makes many of these identifications worthless.
Seite 166 - Rowland remarks that of the fifteen elements named as not found in the sun, many are so classed because they have few strong lines, or none at all, in the limit of the solar spectrum as compared by him with the arc. Boron has only two strong lines. The lines of bismuth are compound and too diffuse. Therefore, even in the case of these fifteen elements, there is little evidence that they are really absent from the sun.