REVIEW: Revision of Rowland's Preliminary Table of Solar Spectrum Wave-Lengths with an Extension to the Present Limit of the Infra-Red by C. E. St. John, C. E. Moore, L. M. Ware, E. F. Adams, H. D. Babcock

1932 ◽  
Vol 75 ◽  
pp. 274
Author(s):  
P. C. Keenan
Keyword(s):  
Solar Spectrum ◽  
Infra Red

scholarly journals II. The wave-lengths of A, a , and of prominent lines in the infra-red of the solar spectrum

1883 ◽  
Vol 36 (228-231) ◽  
pp. 137-138
Keyword(s):  
Solar Spectrum ◽  
Ultra Violet ◽  
Infra Red

M. Fievez has recently sent me a map of the solar spectrum from C to A* inclusive, and as part of this region is one which I have been measuring, I have examined the new publication with great interest. Photography and eye measurements do not exactly coincide in the detail of the grouping of the little a group as far as A, and A itself is shown by M. Fievez’s map as wanting some details which appear in the photographs. Thus in the photographs there are some seventeen lines, whilst in M. Fievez’s map there are but thirteen. Between A and a there are several lines of marked intensity in the photograph which are not shown in the new map. The wave-lengths of the different lines from above “ a ” to A are not the same as those given by Fievez, when they are taken from comparison photo-graphs of the 1st order of the red and 2nd of the ultra-violet on the same plate, or when checked by photographs of the 2nd order of the red with the 3rd order of the green taken in a similar manner. In my paper, “Phil. Trans.,” Part II, 1880, I gave a method of using mirrors by which this could be effected, but since Professor Rowland introduced his concave gratings this is much more readily carried out. He has kindly furnished me with gratings for the purpose, having about 14,400 lines to the inch, with focal distances of 7 feet 6 inches and 12 feet 6 inches respectively. These have been employed in determining the wave-lengths of this part of the spectrum. Cornu’s map was used as a reference for the ultra-violet wave-lengths, and Ångström’s map for those in the blue and green. The two maps may be taken as equally exact. The determination of A has been made by Maseart, Smyth, and others, besides Ångström and Langley, with discordant results. I think the above may be taken as accurate as are Cornu’s and Ångström maps.

High-resolution spectroscopy of minor atmospheric constituents

1956 ◽  
Vol 236 (1205) ◽  
pp. 159-160
Keyword(s):  
Absorption Spectrum ◽  
Vibrational Frequency ◽  
Solar Spectrum ◽  
Resolving Power ◽  
High Resolution Spectroscopy ◽  
Survey Article ◽  
Royal Observatory ◽  
Infra Red ◽  
Scientific Station ◽  
The University

In a recent survey article, Goldberg (1954) gives a list of 127 molecular bands which have been observed in the absorption spectrum of the earth’s atmosphere by studying the solar spectrum between 0.3 and 24 μ . Among these, 35 bands are attributed to the following molecules: O 3 , N 2 O, CH 4 , HDO, CO. The main purpose of this contribution to the Discussion was to show several of these bands as they appear on solar spectrograms taken at the International Scientific Station, Jungfraujoch (Switzerland), in collaboration with Dr L. Neven of the Royal Observatory, Uccle (Belgium). The altitude of this station is 3580 m. It has been pointed out in earlier notes (Migeotte & Neven 1952 a, b ) that these data have been obtained, under high resolving power, by using the prism-grating infra-red spectrograph of the University of Liege (Migeotte 1945). Between 9.33 and 10.08 μ , our spectrograms show 320 lines which are mainly due to the fine structure of the 9.6 μ band of ozone (Migeotte, Neven & Vigroux 1952). Part of our data has been analyzed recently by Kaplan (1955), of the Institute for Advanced Study in Princeton (N. J.), U. S. A. A good fit for low J has been obtained with the following upper-state parameters: vibrational frequency v 3 1042.16 cm -1 ; rotational constants: A = 3.502 1 cm -1 , B = 0.440 1 cm -1 , C = 0.388 3 Cm -1 ; δ = 0.0166 34 .

scholarly journals I. On the new gas obtained from uraninite. Fourth note

1895 ◽  
Vol 58 (347-352) ◽  
pp. 192-192
Keyword(s):  
Wave Length ◽  
Solar Spectrum ◽  
First Order ◽  
Infra Red ◽  
Chromospheric Line

Continued experiments on the gases obtained by heating the minerals bröggerite and euxenite in vacuo have revealed the presence in the spectrum of an important line in the infra-red. By comparisons with the solar spectrum in the first order grating spectrum, the wavelength of the line has been approximately determined as 7065. There can be little doubt, from the observations which have been made, that this new line is coincident with a chromospheric line which occurs in Young’s list, having a frequency of 100, of which the wave-length on, Row land’s scale is stated to be 7065·5.

scholarly journals Photography of the Infra-Red Solar Spectrum to Wave-length 12,900 A

Nature ◽  
1934 ◽  
Vol 133 (3368) ◽  
pp. 759-759 ◽  
Author(s):  
G. HERZBERG
Keyword(s):  
Wave Length ◽  
Solar Spectrum ◽  
Infra Red

scholarly journals New identifications in the infra-red solar spectrum.

1948 ◽  
Vol 54 ◽  
pp. 45 ◽  
Author(s):  
Marcel V. Migeotte
Keyword(s):  
Solar Spectrum ◽  
Infra Red

A Study of the Infra-Red Solar Spectrum with the Interferometer

1927 ◽  
Vol 65 ◽  
pp. 140 ◽  
Author(s):  
Harold D. Babcock
Keyword(s):  
Solar Spectrum ◽  
Infra Red
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