scholarly journals Intensity distribution in the line emission spectrum of cesium

1936 ◽  
Vol 17 (1) ◽  
pp. 45 ◽  
Author(s):  
Fred L. Mohler
2011 ◽  
Vol 59 (5) ◽  
pp. 3014-3018
Author(s):  
Okgyun Kang ◽  
Kyungdeuk Park ◽  
Young-sun Choi ◽  
Wonwook Lee ◽  
Cha-hwan Oh

1998 ◽  
Vol 16 (1) ◽  
pp. 61-70 ◽  
Author(s):  
A. Magunov ◽  
A. Faenov ◽  
I. Skobelev ◽  
T. Pikuz ◽  
D. Batani ◽  
...  

Time- and space-integrated emission spectra measurements have been performed in plasma produced by 308 nm wavelength XeCl laser radiation (IL = (4–10)·1012 W/cm2, τ = 10 ns) and by 248 nm wavelength KrF laser pulse train radiation (IL = 5·1015 W/cm2, τ = 7 ps, 16 pulses in train) on CF2 plane target. Theoretical modelling of Lyman series and He-like ion resonance series of fluorine and its fit of experimental data show considerable differences in the absorption of laser radiation in the two plasmas.


The term “halogen molecule” is intended to include the interhalide compounds as well as the elementary molecules. The existence of three of the ten possible molecules of this type, namely, IF, BrF, and CIF, has not yet been established, and we have not attempted any spectroscopic search for them. For F 2 the data are meagre, only an emission spectrum being known, and we have therefore confined our attention to the other six molecules, namely, CI 2 , Br 2 , I 2 , BrCl, ICI, and IBr. The spectra of these, with the exception of BrCl, have been extensively investigated, and partially interpreted. There are certain features, however, notably the continua and diffuse bands observed in emission, which have not yet been satisfactorily explained, and we have set out to survey the existing data systematically and, where necessary, to obtain new data with the object of accounting for these features. The problem of obtaining satisfactory data of continua and diffuse bands is definitely different from that involved in the case of line and ordinary band spectra. Not only is it more difficult to make accurate visual settings for the purpose of wave-length determinations, but it becomes of much more importance to record the intensity distribution, which is often very characteristic and undoubtedly significant. For these reasons we have thought it essential to obtain and reproduce microphotometer records in all experiments, and to determine wave-lengths solely from these records. Quite low dispersion has been used, and appears very suitable for a general survey, although a more detailed investigation using higher dispersion may well prove profitable later. It seemed important to us to get strictly comparable data in all observations, and it has therefore been necessary to redetermine some of the existing data, which although numerous are seldom complete or homogeneous. A number of entirely new data are also presented. Some consideration must first be given to the known band systems of these molecules, since they provide evidence relating to the location and characteristics of molecular levels, some at least of which may be expected to be concerned in the emission of the continua and diffuse bands.


2020 ◽  
Vol 640 ◽  
pp. A99
Author(s):  
R. Middei ◽  
P.-O. Petrucci ◽  
S. Bianchi ◽  
F. Ursini ◽  
M. Cappi ◽  
...  

Context. Joint XMM-Newton and NuSTAR multiple exposures allow us to disentangle the different emission components of active galactic nuclei (AGNs) and to study the evolution of their different spectral features. In this work, we present the timing and spectral properties of five simultaneous XMM-NewtonandNuSTAR observations of the Narrow Line Seyfert 1 galaxy Mrk 359. Aims. We aim to provide the first broadband spectral modeling of Mrk 359 describing its emission spectrum from the UV up to the hard X-rays. Methods. We performed temporal and spectral data analysis, characterising the amplitude and spectral changes of the Mrk 359 time series and computing the 2–10 keV normalised excess variance. The spectral broadband modelling assumes the standard hot Comptonising corona and reflection component, while for the soft excess we tested two different models: a warm, optically thick Comptonising corona (the two-corona model) and a reflection model in which the soft-excess is the result of a blurred reflected continuum and line emission (the reflection model). Results. High and low flux states were observed during the campaign. The former state has a softer spectral shape, while the latter shows a harder one. The photon index is in the 1.75–1.89 range, and only a lower limit to the hot-corona electron temperature can be found. A constant reflection component, likely associated with distant matter, is observed. Regarding the soft excess, we found that among the reflection models we tested, the one providing the better fit (reduced χ2 = 1.14) is the high-density one. However, a significantly better fit (reduced χ2 = 1.08) is found by modelling the soft excess with a warm Comptonisation model. Conclusions. The present analysis suggests the two-corona model as the best scenario for the optical-UV to X-ray emission spectrum of Mrk 359.


1989 ◽  
Vol 44 (1) ◽  
pp. 81-83 ◽  
Author(s):  
K. Kynev ◽  
V. Kuk

Abstract It is shown that a ZnS:Eu phosphor with line emission spectrum can be prepared without coactivator introduction, contrary to previous results. The broad-band emission established in ZnS: Eu, Li is ascribed to the formation of Eu2+ centres due to the removal of lattice stress by lithium incorporation.


1996 ◽  
Vol 169 ◽  
pp. 497-498
Author(s):  
H. Okuda ◽  
T. Nakagawa ◽  
H. Shibai ◽  
Y. Doi ◽  
K. Mochizuki ◽  
...  

An extensive survey of [C II] line emission at 158 microns using the balloon borne telescope (BICE) has provided a complete map of the emission intensity distribution in the first and the fourth quadrants of the galactic plane (280° < l < 80°, −5° < b < 5°: Okuda et al. 1993). The emission is very extended throughout the galactic plane in which three intensity maxima are seen towards the tangential directions of the Scutum and the Norma arms as well as in the Galactic center region. However the Galactic center maximum is much less prominent compared with the two other distributions, unlike the case of far infrared continuum and CO emissions.


1970 ◽  
Vol 13 (4) ◽  
pp. 1304-1306 ◽  
Author(s):  
N. E. Kuz'menko ◽  
Yu. Ya. Kuzyakov ◽  
A. D. Smirnov

1986 ◽  
Vol 119 ◽  
pp. 295-306
Author(s):  
S. Collin-Souffrin

Our knowledge of the physical conditions and of the structure of the broad line emissive region -the BLR- is reviewed. First we derive the model independent constraints on the different zones emitting the broad lines. Then we discuss photoionized models. In a first step the BLR is assumed to be made only of one type of cloud emitting all the broad lines. We show that this model is unable to explain the observed spectrum. We thus assume that the high and low ionization lines are emitted by different clouds, still photoionized. This assumption is also in contradiction with the observations and we are led to the idea of a large variety of emitting clouds. Finally the hypothesis of a purely radiative heating mechanism should also be questioned.


1977 ◽  
Vol 55 (2) ◽  
pp. 180-188 ◽  
Author(s):  
J.-L. Féménias ◽  
J. P. Goure ◽  
R. Stringat

Previous work on the theoretical study of the intensity distribution in the emission spectrum of ScO is now extended and a comparison is made with some experimental spectrometric data, and some physical results such as the temperature of emission and the 'spin allowed' property of the A2Π → X2Σ transition are given and discussed. The great influence of the slight spin decoupling of the A2Π (case (a)) state on the intensity distribution is shown and is explained theoretically using the mixing coefficients obtained in a former rotational study of the spectrum.


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