Off-axis line profiles of atomic-oxygen resonance lamps used in the upper atmosphere

1985 ◽  
Vol 34 (3) ◽  
pp. 271-273
Author(s):  
D.B. Jenkins ◽  
D.P. Wareing
Keyword(s):  
Atomic Oxygen ◽  
Upper Atmosphere ◽  
Line Profiles

Resolved line profiles of atomic oxygen resonance lamps used in the upper atmosphere

1985 ◽  
Vol 34 (2) ◽  
pp. 123-132 ◽  
Author(s):  
D.B. Jenkins ◽  
G. Watkin ◽  
D.P. Wareing ◽  
G.H.C. Freeman ◽  
P.H.G. Dickinson ◽  
...  
Keyword(s):  
Atomic Oxygen ◽  
Upper Atmosphere ◽  
Line Profiles

Silver Film Atomic Oxygen Sensors: Further Evidence for Utility as an Atmospheric Probe

1974 ◽  
Vol 52 (21) ◽  
pp. 2174-2175 ◽  
Author(s):  
W. R. Henderson
Keyword(s):  
Atomic Oxygen ◽  
Silver Film ◽  
Oxygen Sensors ◽  
Rate Of Change ◽  
Upper Atmosphere ◽  
Silver Films

Further evidence for the utility of thin silver films as detectors of atomic oxygen in the upper atmosphere is given. Measurements show that under prescribed conditions no correction for rate of oxidation or rate of change of oxidation is necessary.

scholarly journals Mariner 6: Ultraviolet spectrum of Mars upper atmosphere

1971 ◽  
Vol 40 ◽  
pp. 253-256 ◽  
Author(s):  
C. A. Barth ◽  
W. G. Fastie ◽  
C. W. Hord ◽  
J. B. Pearce ◽  
K. K. Kelly ◽  
...  
Keyword(s):  
Carbon Dioxide ◽  
Carbon Monoxide ◽  
Spectral Region ◽  
Atomic Hydrogen ◽  
Atomic Oxygen ◽  
Ultraviolet Spectrum ◽  
Upper Atmosphere

Emission features from ionized carbon dioxide and carbon monoxide were measured in the 1900- to 4300-Å spectral region. The Lyman-α 1216-Å line of atomic hydrogen and the 1304-, 1356-, and 2972-Å lines of atomic oxygen were observed.

scholarly journals Photodissociation of Carbon Dioxide in the Mars Upper Atmosphere

1974 ◽  
Vol 29 (2) ◽  
pp. 185-188
Author(s):  
Charles A. Barth
Keyword(s):  
Carbon Dioxide ◽  
Carbon Monoxide ◽  
Atomic Oxygen ◽  
Emission Rate ◽  
Upper Atmosphere ◽  
Emission Rates ◽  
Laboratory Measurements

Photodissociation of carbon dioxide produces O (1S) atoms and CO (a3Π) molecules in the Mars upper atmosphere. Calculations of the emission rate of the atomic oxygen 2972 Å line and the carbon monoxide Cameron bands produced by the photodissociation mechanism are factors of 3 and 10, respectively, smaller than the emission rates observed by Mariner ultraviolet spectrometers. Laboratory measurements are needed to understand the discrepancies.

Method of monitoring atomic oxygen and molecular nitrogen composition in the upper atmosphere on XUV images of the Sun

2010 ◽  
Vol 50 (5) ◽  
pp. 679-685 ◽  
Author(s):  
V. G. Mordovskaya ◽  
A. P. Ignat’ev ◽  
S. I. Boldyrev ◽  
S. A. Boldyrev ◽  
G. S. Ivanov-Kholodnyi ◽  
...  
Keyword(s):  
Atomic Oxygen ◽  
Molecular Nitrogen ◽  
Upper Atmosphere ◽  
The Sun

scholarly journals Upper thermospheric ion-neutral coupling from combined optical and radar experiments over Svalbard

2009 ◽  
Vol 27 (11) ◽  
pp. 4293-4303 ◽  
Author(s):  
E. M. Griffin ◽  
A. L. Aruliah ◽  
I. McWhirter ◽  
H.-C. I. Yiu ◽  
A. Charalambous
Keyword(s):  
Experimental Data ◽  
Northern Hemisphere ◽  
Atomic Oxygen ◽  
Numerical Models ◽  
Laboratory Data ◽  
Upper Atmosphere ◽  
Unique Combination ◽  
Rapid Changes ◽  
Spatially Extended

Abstract. The response of thermospheric neutral parameters such as winds and temperatures to rapid changes in geophysical conditions has usually been considered to be relatively slow, on the order of hours, and steady, representing an integration of more rapid ionospheric changes. Quantifying the relevant ion-neutral coupling has proved difficult due to a lack of relevant laboratory data for the most important collisions, namely between neutral atomic oxygen and its first ion. As a result the representation of ion-neutral coupling in numerical models of the upper atmosphere has often produced poor comparison to experimental data. Using a unique combination of spatially extended ion and neutral thermospheric parameters we show that the neutral response can be very rapid, within 15 min, to imposed forcing via ion-neutral coupling. The array of complementary instrumentation measuring the thermosphere above Svalbard in the Northern Hemisphere allows detailed study of the causes and effects from both the ion and neutral perspectives. The implications for development and testing of the thermospheric numerical models is discussed.

The Composition Of The Upper Atmosphere According to The Dissociation Of Oxygen And Nitrogen Molecules

1944 ◽  
Vol 25 (6) ◽  
pp. 245-250 ◽  
Author(s):  
J. Gauzit
Keyword(s):  
Solar Radiation ◽  
Atomic Oxygen ◽  
Atomic State ◽  
Upper Atmosphere ◽  
Night Sky ◽  
Ultraviolet Solar Radiation

We show that the observation of forbidden lines in the spectra of the night sky and of aurorae requires that the upper atmosphere should be composed essentially of atomic oxygen and nitrogen. The transition between molecular and atomic regions is realized abruptly for both gases towards the height of 100 km. The absorption of the ultraviolet solar radiation undoubtedly decomposes the oxygen molecules of the upper atmosphere, but the dissociation of nitrogen molecules is harder to understand. Molecular recombinations by triple collisions being unusual in the upper altitudes, we can understand that a weak dissociative source is able to maintain the atomic state of upper atmospheric layers: the most probable one is photochemical dissociation, but the effect is important only when the temperature rises above 1000° K.

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