The Chemistry of the Sun |
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Common terms and phrases
absorption already appearance atmosphere atomic bands become blue bodies bright lines calcium CHAPTER chemical coincident coloured compared complex compound considerable continuous dark dealing determine eclipse effect electric elements employed evidence examined exist experiments fact flame Fraunhofer further give given glass greater green groups higher hydrogen hypothesis important increased indicated intensity iron lines Kirchhoff length less light lower magnesium matter means metallic method molecules nature observed obtained origin pass phenomena photographs photosphere poles position possible present prism produced prominences question rays recorded referred refrangible regard region represented result reversed seen short showing shown side slit sodium solar spectrum spark spectra spectroscope spots stars substances sun-spot sun's temperature thickness tube vapour various vary vibrations visible wave-length widened yellow
Popular passages
Page 245 - It is abundantly clear that if the so-called elements, or more properly speaking their finest atoms — those that give us line spectra — are really compounds, the compounds must have been formed at a very high temperature. It is easy to imagine that there may be no superior limit to temperature, and therefore no superior limit beyond which such combinations are possible...
Page 52 - ... or both of those fundamental modes, if some of the incident light is of one or other of their periods, or some of one and some of the other; so that the energy of the waves of those particular qualities of light is converted into thermal vibrations of the medium and dispersed in all directions, while light of all other qualities, even though very nearly agreeing with them, is transmitted with comparatively no loss. (5) That...
Page 174 - ... this latter being invariably thicker than the H lines in all photographs of the calcium spectrum, and remaining, moreover, visible in the spectrum of substances containing calcium in such small quantities as not to show any traces of the H lines. " How far this and similar variations between photographic records and the solar spectrum are due to causes incident to the photographic record itself, or to variations in the intensities of the various molecular vibrations under solar and terrestrial...
Page 207 - we may conceive that in remote ages the temperature of matter was much higher than it is now, and that these other things [the ideal elements] existed in the state of perfect gases — separate existences — uncombined." He further suggested, from spectroscopic evidence, that it is probable that "we may one day.
Page 166 - That occasionally photospheric matter appears to be injected into the chromosphere. May not these facts indicate that the absorption to which the reversal of the spectrum and the Fraunhofer lines are due takes place in the photosphere itself or extremely near to it, instead of in an extensive outer absorbing atmosphere ? And is not this conclusion strengthened by the consideration that FIRST otherwise the newly-discovered bright lines in the solar FAPER' spectrum itself should be themselves reversed...
Page v - It is conceivable that the various kinds of matter, now recognized as different elementary substances, may possess one and the same ultimate or atomic molecule existing in different conditions of movement.
Page 11 - The line A that bounds the red side of the spectrum is somewhat confused, which seems in part owing to want of power in the eye to converge red light. The line B, between red and green, in a certain position of the prism, is perfectly distinct; so also are D and E, the two limits of violet. But C, the limit of green and blue, is not so clearly marked as the rest ; and there are also, on each side of this limit, other distinct dark lines, / and g, either of which, in an imperfect experiment, might...
Page 135 - If the hydrogen-lines were invariably observed to broaden out on both sides, the idea of movement would require to be received with great caution ; we might be in presence of phenomena due to greater pressure, both when the lines observed are bright or black upon the sun ; but when they widen out sometimes on one side, sometimes on the other, and sometimes on both, this explanation appears to be untenable, as Dr. Frankland and myself in our researches at the College of Chemistry have never failed...
Bibliographic information
| Title | The Chemistry of the Sun Landmarks of science Nineteenth Century Collections Online (NCCO): Science, Technology, and Medicine: 1780-1925 |
| Author | Sir Norman Lockyer |
| Publisher | Macmillan and Company, 1887 |
| Length | 457 pages |
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