Atmospheric structure

This wavelength is in the UV region, and it does not reach the surface of the Earth. 

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The formation of photochemically driven layers in the atmosphere, such as the ozone hole a natural consequence of atmospheric structure... 

Atmospheric structure Composition of N2 and CH4 with a complex hydrocarbon/Chapman layer structure... 

Trafton has shown in 1964 that the opacity in the far infrared of the atmospheres of the outer planets is due to the rototranslational band of H2-H2 and H2-He pairs [393], It is now clear that collision-induced absorption plays a major role in the thermal balance and atmospheric structure of the major planets. The Voyager emission spectra of Jupiter and Saturn show dark fringes in the vicinity of the So(0) and So(l) lines of H2, Fig. 7.3, which are due to collision-induced absorption in the upper,... 

ABSTRACT. From the analysis of the galactic counterparts of the HS variables/tjCar, AG Car and P Cyg we conclude that their atmospheres are near critical physical conditions so that small changes of the mass outflow could produce a large variation of the atmospheric structure and nova-like explosions at nearly constant Mbol. 

In this contribution, we first examine the known mass-loss mechanisms in the light of the recent observations(Sect.II),and then we review some recent infrared and radio observations that may be relevant to our understanding of the outer atmospheric structure and mass-loss phenomena(Sect.Ill). Based on these observations, new picture of the outer atmosphere of red (super)giant stars is proposed and its implications on circumstellar chemistry as well as on mass-loss phenomena are discussed(Sect.IV). 

While the intensity anomaly alone(item 1 above) can be due to our poor understanding of atmospheric structure and/or of line formation in the upper atmosphere, peculiar line shift and line asymmetry(item 2) as well as differential time variation note above(item 3) suggest that at least a part of low excitation lines should be originating not in the photosphere but in an extra layer well separated from the photosphere. We tentatively refer this separate extra layer as CO absorption layer (the "layer" does not necessarily imply that it is well stratified but rather it can also be an inhomogeneous component in outer atmosphere, and the "layer" is used in this extended meaning in what follows). 

In the third section, we review recent developments in the field of atmospheric free radical observations so we can explore how effectively these experiments have tested our understanding of atmospheric structure. The fourth section summarizes this progress and then presents the latest predictions of global ozone depletion resulting from fluorocarbon release. Recent and important changes have been reported in this aspect of the problem. 

June 14, 1967 Mariner 5, flyby Oct. 19, 1967 flyby (3,900 km), atmospheric structure composition expts. see Jastrow and Rasool (1969)... 

Yelle R. V., Lunine 1.1., Pollack J. B., and Brown R. H. (1996) Lower atmospheric structure and surface-atmospheric interaction on Triton. In Neptune and Triton (ed. D. Cruikshank). University of Arizona Press, Tucson, pp. 1031-1106. 

Lack of an abundance estimate for a trace element like boron has no effect on the accuracy of the abundance analysis for other elements but merely restricts astrophysical interpretations involving B. On the other hand, helium is an abundant elements with effects on the atmospheric structure and through this on the derived abundances of other elements. Although rarely stated explicitly, abundance analyses of cool stars are dependent on an assumption about the He/H ratio the assumption enters both into the model atmosphere and synthetic spectrum calculations. For normal stars, ignorance about the He/H ratio is mitigated by the fact that the He/H ratio is surely constrained within tight limits (Y = 0.24 to 0.26, see above). 

The atmosphere structure may be considered from different standpoints. A classification frequently accepted is that connected with change in the vertical direction i.e. the vertical arrangement of the atmosphere in layers dependent on temperature, changes of the air composition at different altitudes, etc. 

The vertical change of the pressure is much larger than its horizontal or time variability. Thus, it is convenient to define a standard atmosphere [7], which represents the atmospheric structure averaged with respect to time and to the horizontal direction and varying only with height changes. 

Electrostatic interactions give a large deviation from ideality in equilibrium properties of solutions containing low molecular weight electrolytes. This deviation was most successfully disposed of by the Debye-Huckel theory [2]. According to this theory, the ionic species are not distributed in solution in a random manner, but form an ionic atmosphere structure, and the thermodynamic properties such as the activity coefficient of solvent (or the osmotic coefficient), the mean activity coefficient of solute, and the heat of dilution, decrease linearly with the square root of the concentration, in conformity with experimental observations. 

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