The Chemistry of the Sun

Front Cover
Macmillan and Company, 1887 - 457 pages
 

Contents

Fraunhofers Theodolite Spectroscope
15
THE FIRST GLIMPSES OF 66 BRIGHT LINE SPECTRA
23
Showing Arrangement of Slit and Prism
24
Introduction of a Lens to Produce an Image
25
Directvision Prism with three Prisms showing Path of Ray
27
Improvised Bunsen Burner
28
Method of Inserting Platinum Wire and Salt into Flame
29
The Spectra of Continuous and Discontinuous Light Sources the latter seen with a Line and Circular Slit
31
The Spectrum of a Complicated Light Source as seen with a Circular and a Line Slit
32
BREWSTER HERSCHEL AND FORBES BECQUEREL AND DRAPER 18221843
34
Copies of Herschels Absorption Diagrams
36
Diagram showing the increasing thickness of Air through which the Light of the Sun has to pass as it descends towards the horizon
38
Absorption of Sunlight by various thicknesses of a Solution of the Salts of Chromium Gladstone
40
Method of Studying the Absorption of Iodine Vapour
41
Reduced Copy of Becquerels Photograph of the Complete Solar
47
THE FRAUNHOFER LINES EXPLAINED
49
Diagram showing the Solar Spectrum and the Bright Double Line D
55
Diagram illustrating the Graphical Formulæ employed on p
63
KIRCHHOFFS MAP AND WORK
69
Spectroscope with Reflected Scale
70
THE WORK OF ÅNGSTRÖM AND THALEN
83
Ångströms Spectrometer
85
VIIIA NEW METHOD OF WORK
94
Sunspot Secchi
95
Mr Hastingss Arrangement for Comparison of Spectra
103
MORE RESULTS OF THE NEW METHOD
106
Spectrum of the Suns Photosphere and Chromosphere showing the Lines
111
Edge of Chromosphere billowy
117
FIG PAGE 51 The same Prominence fifteen minutes afterwards
118
Noncoincidence of Bright and Dark F Line
119
Contortions of F Line in a Prominence
120
Contortions of the Hydrogen Lines
121
Spectrum of Sodium showing the Long and Short Lines
145
Arrangement for Projecting the Long and Short Lines on a Screen
146
Copy of Dr Millers Spectrum of Cadmium showing the Dots
147
SOME RESULTS OF THE LONG AND SHORT METHOD
150
DIFFICULTIES
161
The Sun and its Atmosphere on Kirchhoffs Hypothesis
163
Diagram showing that if the Suns Atmosphere consists of Layers the Lines will extend down to the Solar Spectrum
164
Imagined Stratification of the Solar Atmosphere
169
Stratification of the Solar Atmosphere Disturbed by the Upheaval of a Prominence
170
Fluted Spectrum of Iodine Thalèn
180
DETAILS OF SOME OF THE DIFFICULTIES
182
Hugginss Stellar Spectra
188
Three Chief Types of Stellar Spectra
189
The Varying Intensities of the Lines of Calcium as seen under different conditions
194
Various Intensities of the Lines of Magnesium as seen under different conditions
196
Showing the Various Intensities of the Lines of Lithium under different conditions
197
A POSSIBLE WAY OUT OF THEM
199
INTRODUCTION OF PHOTOGRAPHY
209
Wavelength Map of the Solar Spectrum
210
A STUDY OF THE PURIFIED SPECTRA
229
DISCUSSION OF THE DISSOCIATION HYPOTHESIS
237
DISCUSSION OF THE DISSOCIATION HYPOTHESIS continued
259
SOME TEST EXPERIMENTSABSORPTION PHENOMENA
273
SOME TEST EXPERIMENTSTRIAL OF NEW METHODS
290
CHAP PAGE XXII THE SOLAR ATMOSPHERE ON THE NEW HYPOTHESIS
303
MORE TESTSTHE SPECTRA OF SUNSPOTS
310
SPECIAL TESTS WITH REGARD TO IRON
326
TESTS SUPPLIED BY ECLIPSE OBSERVATIONS
354
THE BASIC LINES
368
TESTS SUPPLIED BY THE PHENOMENA OF THE ARC
378
APPLICATIONS OF THE HYPOTHESIS TO THE GENERAL PHENO MENA OF THE SUN
402
INDEX
450

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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...

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