Collision-produced Na2 diffuse violet band

1979 ◽  
Vol 28 (1) ◽  
pp. 78-80 ◽  
Author(s):  
A. Kopystyńska ◽  
P. Kowalczyk
Keyword(s):  
Author(s):  
R. Freitag ◽  
K. Thonke ◽  
R. Sauer ◽  
D. G. Ebling ◽  
L. Steinke

We report on the time-resolved luminescence of the defect-related violet band from undoped AlN epitaxial layers grown on sapphire and SiC. For both measurements in photoluminescence and in cathodoluminescence a decay of algebraic nature at long times is observed. This is typical for donor-acceptor pair transitions. We compare the behavior of this band to that of the generically yellow luminescence of GaN.


1968 ◽  
Vol 48 (5) ◽  
pp. 1980-1984 ◽  
Author(s):  
F. J. LeBlanc
Keyword(s):  

2018 ◽  
Vol 20 (4) ◽  
pp. 209-217
Author(s):  
S.S. Kurbanov ◽  
Sh.Z. Urolov ◽  
Z.Sh. Shaymardanov ◽  
R.R. Jalolov

Room temperature photoluminescence (PL) properties of vertically aligned and spindle-shaped, randomly oriented ZnO nanorods synthesized by using a low temperature hydrothermal method are studied. In air, the vertically aligned ZnO nanorods oriented mainly parallel to the luminescencerecording axis exhibited only one, very strong UV emission peak at 382 nm. This band is assigned to emission of free excitons. A new violet PL band near 400 nm arises with increasing angle between the nanorod growth direction and the luminescence-recording axis. The violet band also appears under UV illumination in vacuum and vanishes after exposure to air. The randomly oriented ZnO nanorods along with free exciton related PL band reveal a broad yellow-orange emission band around 590 nm. The violet band is attributed to Zn vacancy related defects or their complexes, while the yellow-orange emission band is ascribed to oxygen interstitial related defects.


1997 ◽  
Vol 36 (Part 2, No. 10A) ◽  
pp. L1301-L1303 ◽  
Author(s):  
Da Xing ◽  
Qi Wang ◽  
Shi-ci Tan ◽  
Ken-ichi Ueda

1928 ◽  
Vol 68 ◽  
pp. 257 ◽  
Author(s):  
R. T. Birge ◽  
J. J. Hopfield

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

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).


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

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.


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