Differences in near UV /approximately 3400-4300 A/ optical emissions from midday cusp and nighttime auroras

Details Differences in near UV /approximately 3400-4300 A/ optical emissions from midday cusp and nighttime auroras Differences in near UV /approximately 3400-4300 A/ optical emissions from midday cusp and nighttime auroras

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983jgr....88..435s&link_type=abstract

Journal of Geophysical Research, vol. 88, Jan. 1, 1983, p. 435-441.

Physics

25

Auroral Spectroscopy, Auroras, Near Ultraviolet Radiation, Night Sky, Optical Emission Spectroscopy, Ultraviolet Spectroscopy, Charge Exchange, Energy Dissipation, Ionic Reactions, Nitrogen Ions, Particle Energy, Resonance Scattering

Scientific paper

The near-UV spectroscopic properties of emissions from high-altitude (over 200 km) midday cusp auroras, in which low-energy particles dissipate energy in reacting with atomic species in the thermosphere, are compared with those of the low-altitude (about 110 km) nighttime auroras, representing the precipitation of keV particles into regions where molecular species are abundant. Measurements were made in the region 3400-3900 A from Spitsbergen island (geomagnetic latitude 75 deg N) near winter noon, and from Fairbanks, Alaska (geomagnetic latitude 64.6 deg N) during the night. The nighttime emissions are found to consist mostly of N2 2P, N2 VK and N2(+) 1NG bands, while midday cusp auroral emissions are largely devoid of molecular emissions, with atomic emissions from metastable species predominant. An excess of N2(+) 1NG emission with respect to calculations of the interactions of low-energy electrons with atmospheric N2 and in situ particle measurements is obtained which is attributed to the resonant scattering of sunlight by N2(+) ions formed in a charge exchange reaction. The observation of He 3889-A in the midday cusp region is also noted, along with the forbidden O II 3726-29 A emission, which has been detected only once at night.

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