Other
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsa53b1378k&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #SA53B-1378
Other
0300 Atmospheric Composition And Structure, 0310 Airglow And Aurora, 0355 Thermosphere: Composition And Chemistry, 0394 Instruments And Techniques, 0399 General Or Miscellaneous
Scientific paper
The principal optical observable resulting from ionospheric modification (IM) experiments is the oxygen red line at 630 nm, originating with the O(^1D - 3P) transition. Because the O(^1D) atom has a radiative lifetime of 110 s, it is very sensitive to collisional quenching, and a decay faster than the radiative rate can be attributed to collisions with other atmospheric particles. At the typical energy deposition altitudes of 220-300 km, the predominant collider is O(3P), with lesser amounts of N2. The O(^1D) + N2 rate coefficient is well known, but until recently there was no direct knowledge of the effect of O(3 P) as an O(^1D) quencher. New laboratory experiments have shown it to be very efficient, with almost the same rate coefficient as N2, leading to the conclusion that the dominant quencher in IM experiments is O(3P). It follows that measurement of 630 nm decay provides a measure of the O(3P) density in the excited region. Over the last 35 years a number of IM experiments have been reported. With knowledge of the O(^1D) + O(3P) rate coefficient, we are able to compare the results of these studies with atmospheric composition models, realizing that the energy is absorbed over some altitude range. We present data that have been accumulated from a number of IM sites [HAARP, SURA, Platteville, EISCAT] to show that it is generally possible to map out overhead O(3P) by this method.
Kalogerakis Konstantinos S.
Kendall E. A.
Slanger Tom G.
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