Some New Ultra-violet Band Systems of Selenides and Tellurides of Tin and Lead

Nature ◽  
1946 ◽  
Vol 157 (3994) ◽  
pp. 663-663 ◽  
Author(s):  
DEVENDRA SHARMA
Keyword(s):  
Ultra Violet ◽  
Violet Band

The Ultra-Violet Band Spectrum of Nitrogen

1928 ◽  
Vol 68 ◽  
pp. 257 ◽  
Author(s):  
R. T. Birge ◽  
J. J. Hopfield
Keyword(s):  
Ultra Violet ◽  
Band Spectrum ◽  
Violet Band

Ultra-Violet Band System of Silicon Monoselenide

Nature ◽  
1938 ◽  
Vol 142 (3592) ◽  
pp. 434-434 ◽  
Author(s):  
R. F. BARROW
Keyword(s):  
Band System ◽  
Ultra Violet ◽  
Violet Band

scholarly journals The ultra-violet band-system of carbon monosulphide and its relation to those of carbon monoxide ( the “4th positive” bands) and silicon monoxide

1928 ◽  
Vol 117 (777) ◽  
pp. 351-375 ◽  
Keyword(s):  
Band System ◽  
Carbon Disulphide ◽  
Ultra Violet ◽  
Silicon Monoxide ◽  
Positive System ◽  
Quantum Analysis ◽  
Constant Change ◽  
Group A ◽  
Carbon Arc ◽  
Violet Band

In 1913 L. C. Martin discovered an ultra-violet band-system in the tube discharge through carbon disulphide vapour and in the carbon arc fed with sulphur, and ascribed it, on experimental evidence, to the CS molecule. The bands are degraded towards the red, and the majority of them are double headed. Martin arranged all but seven of the observed bands into seven groups (A, B, ... G) each formed by closely neighbouring bands. The present com­munication records the quantum analysis of the band-heads, and the sub­stantial similarity of structure between this CS system, the ultra-violet systemof SiO and the “4th Positive” system of CO. A brief examination of the photographs reproduced by Martin and of the wave-numbers derived from his tabulated wave-lengths leads to a Deslandres scheme for the band-heads and to a plausible assignment of the initial and final vibrational quantum numbers, n ', n ". In this scheme each of Martin’s seven groups is a sequence of bands corresponding to a constant change of vibrational quantum number, n "— n ', except that groups B and C together with one band of group A form only one sequence, n "— n ' = — 2. It further appears that of the pair of heads (bracketed in Martin’s table of data) of each double­ headed band, the less refrangible head is formed by a Q branch, the corresponding P branch having, of course, no head, and therefore remaining undetected with the dispersion employed by Martin (about 7.8 A./mm. at λ 2420 to 12.7 A./mm. at λ 2850).

scholarly journals VI. The ultra-violet band of ammonia, and its occurrence in the solar spectrum

1919 ◽  
Vol 218 (561-569) ◽  
pp. 351-372 ◽  
Keyword(s):  
Solar Spectrum ◽  
Ultra Violet ◽  
Maximum Intensity ◽  
Resolving Power ◽  
The Sun ◽  
Sufficient Detail ◽  
Other Substances ◽  
Violet Band ◽  
Band Spectra

A question of great interest in connection with the solar spectrum is that of the origin of the thousands of unidentified faint lines which were catalogued by Rowland in his “Preliminary Table of Solar Spectrum Wave-lengths.” Some of these lines may possibly be identical with faint lines in metallic spectra which have not yet been completely tabulated, but in view of the presence of bands of cyanogen, carbon and hydrocarbon, the possibility of the correspondence of most of them with band spectra of other substances should not be overlooked. As a contribution to this inquiry, the present investigation was undertaken primarily in order to determine whether Group P in the ultra-violet region of the solar spectrum might not be mainly due to the presence of ammonia in the absorbing atmosphere of the sun. Ammonia was already known to give a remarkable band in this region, having its position of maximum intensity near λ 3360, but it had not been investigated in sufficient detail to permit of an adequate comparison with the solar tables. Photographs have accordingly been taken with spectrographs of high resolving power for the purpose of this comparison, and, as will appear from the details which follow, it has been established that the ammonia band is certainly represented in the solar spectrum, and accounts for a considerable number of faint lines for which no other origins have been suggested.

The Ultra-Violet Band Spectrum of Carbon Monoselenide

1953 ◽  
Vol 66 (9) ◽  
pp. 836-839 ◽  
Author(s):  
R K Laird ◽  
R F Barrow
Keyword(s):  
Ultra Violet ◽  
Band Spectrum ◽  
Violet Band

Ultra-violet band-systems of SiCl

1936 ◽  
Vol 48 (4) ◽  
pp. 563-573 ◽  
Author(s):  
W Jevons
Keyword(s):  
Ultra Violet ◽  
Violet Band

scholarly journals The spectrum of ammonia

1923 ◽  
Vol 103 (723) ◽  
pp. 696-705 ◽  
Keyword(s):  
Visible Region ◽  
Solar Spectrum ◽  
Ultra Violet ◽  
Band Spectrum ◽  
Green Part ◽  
Violet Band ◽  
Vacuum Tubes ◽  
Α Band

A large number of lines in the solar spectrum previously unidentified have been attributed to ammonia by Fowler and Gregory. Their investigation however, referred only to the characteristic ultra-violet band with its centre at about λ 3360, and it seemed desirable to continue the inquiry, in order to determine whether other bands associated with ammonia are also represented in the solar spectrum. One of the bands, in the yellow-green part of the spectrum, about λ 5635, was first observed in vacuum tubes by Schuster, and has since been found to consist of two adjacent bands. Besides this, there is an extended band spectrum ranging through the greater part of the visible region, which appears in the greater part of the visible region, which appears in the flame in the flame of ammonia burning in oxygen, and has been called the "α-band" by Eder and Valenta.

Ultra-violet band systems of silicon monoselenide and monotelluride

1939 ◽  
Vol 51 (2) ◽  
pp. 267-273 ◽  
Author(s):  
R F Barrow
Keyword(s):  
Ultra Violet ◽  
Violet Band
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