scholarly journals EFFECTS OF NITROGEN PHOTOABSORPTION CROSS SECTION RESOLUTION ON MINOR SPECIES VERTICAL PROFILES IN TITAN’S UPPER ATMOSPHERE

2015 ◽  
Vol 801 (1) ◽  
pp. L14 ◽  
Author(s):  
A. Luspay-Kuti ◽  
K. E. Mandt ◽  
S. Plessis ◽  
T. K. Greathouse
Keyword(s):  
Cross Section ◽  
Upper Atmosphere ◽  
Photoabsorption Cross Section ◽  
Vertical Profiles

The absolute N2 K-photoabsorption cross section up to hω = 450 eV

1978 ◽  
Vol 58 (2) ◽  
pp. 263-266 ◽  
Author(s):  
H. Petersen ◽  
A. Bianconi ◽  
F.C. Brown ◽  
R.Z. Bachrach
Keyword(s):  
Cross Section ◽  
Photoabsorption Cross Section ◽  
The Absolute

scholarly journals Estimate of the D/H ratio in the Martian upper atmosphere from the low spectral resolution mode of MAVEN/IUVS

2020 ◽  
Author(s):  
Jean-Yves Chaufray ◽  
Majd Mayyasi ◽  
Michael Chaffin ◽  
Justin Deighan ◽  
Dolon Bhattacharyya ◽  
...  
Keyword(s):  
High Resolution ◽  
Spectral Resolution ◽  
Quantitative Information ◽  
Upper Atmosphere ◽  
Vertical Profiles ◽  
Low Resolution ◽  
Mars Atmosphere

<p>The recent observations performed with the high-resolution “echelle mode” by the Imaging Ultraviolet Spectrograph (IUVS) aboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission indicated large deuterium brightness near Ls=270°. The deuterium brightness observed at the beginning of the mission, when Mars was close to its perihelion show brightness ~ 1 kR much larger than the first deuterium detection from Earth ~ 20-50R in 20-21 January 1997 (Ls = 67°). This low brightness of the deuterium emission is consistent with the lack of deuterium observation with the echelle mode of IUVS at solar longitudes around aphelion (Ls = 71°). During southern summer (Ls = 270°), especially near the terminator, the Lyman-α emission observed at 121.6 nm with the “low resolution mode” presents some vertical profiles that were not reproducible with models including only the emission from the thermal hydrogen population. In this study, we investigate the possibility to derive quantitative information on the D/H ratio at Mars from the vertical Lyman-α profiles observed with the “low resolution mode”, and the main limits of the method.</p>

scholarly journals High-resolution photoabsorption cross-section measurements of SO2at 198 K from 213 to 325 nm

2011 ◽  
Vol 116 (E3) ◽  
Author(s):  
D. Blackie ◽  
R. Blackwell-Whitehead ◽  
G. Stark ◽  
J. C. Pickering ◽  
P. L. Smith ◽  
...  
Keyword(s):  
High Resolution ◽  
Cross Section ◽  
Photoabsorption Cross Section

Solute Dispersion and Sediment Transport in Estuaries

1986 ◽  
Vol 18 (4-5) ◽  
pp. 93-100
Author(s):  
J. R. West ◽  
I. Guymer ◽  
Y. Sangodoyin ◽  
K O. K. Oduyemi
Keyword(s):  
Sediment Transport ◽  
Cross Section ◽  
Transverse Shear ◽  
Suspended Solids ◽  
Vertical Profiles ◽  
Dispersion Coefficients ◽  
Solute Dispersion ◽  
Turbulent Fluctuations ◽  
Solids Transport ◽  
Solids Concentration

Synoptic measurements of velocity and salinity at several points on up to five vertical profiles at a cross-section in the Conwy show that solute dispersion coefficients are affected by secondary flow induced by the interaction of transverse shear and the salinity induced longitudinal density gradient. It is concluded that dispersion coefficients are temporally and spatially dependent and a simple empirical formula is suggested. Some data from the initial stages of a similar study of sediment transport show that techniques exist which permit the study of the turbulent fluctuations of suspended solids concentration and the evaluation of the tidal dependence of suspended solids transport phenomena.

A discussion on infared astronomy - On the chemistry of Jupiter's upper atmosphere

1969 ◽  
Vol 264 (1150) ◽  
pp. 151-151
Keyword(s):  
Ultraviolet Radiation ◽  
Cross Section ◽  
Infrared Radiation ◽  
Organic Molecules ◽  
General Procedure ◽  
Analytical Approximation ◽  
Upper Atmosphere ◽  
Rapid Rise ◽  
Absorption Bands ◽  
Jovian Atmosphere

The infrared opacity of Jupiter’s upper atmosphere will be influenced by line blanketing resulting from strong absorption bands of ammonia and organic molecules. In order to calculate these effects eventually, we conduct a first investigation into the ion-molecule chemistry of the upper Jovian atmosphere. Experimental results show that intense ultraviolet radiation reacts with the constituents of the Jovian atmosphere to produce C2H4> ^2^65 a, and higher polymers. The general procedure for calculating both equilibrium and non-equilibrium abundances of these products is formulated and applied to the case of the surface passage of a satellite shadow. A specific example is made of ethylene, for which an analytical approximation gives 10 (to power of 10) molecules in an atmospheric column of 1 cm2 cross-section after a very rapid rise to equilibrium. Such a concentration of ethylene does not substantially affect the infrared radiation in the shadow.

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