Auroral modeling of the 3371 A emission rate - Dependence on characteristic electron energy

Details Auroral modeling of the 3371 A emission rate - Dependence on characteristic electron energy Auroral modeling of the 3371 A emission rate - Dependence on characteristic electron energy

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....9510337r&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 95, July 1, 1990, p. 10337-10344.

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Airglow, Auroral Zones, Electron Energy, Emission Spectra, Molecular Collisions, Spectral Energy Distribution, Backscattering, Energy Dissipation, Ionization Potentials, Light Emission, Oxygen Atoms, Thermosphere

Scientific paper

An efficient two-stream auroral electron model is used to study the deposition of auroral energy and the dependence of auroral emission rates on characteristic energy. This model incorporates the concept of average energy loss to reduce the computation time. This simple two-stream model produces integrated emission rates that are in excellent agreement with the much more complex multistream model of Strickland et al. (1983) but disagrees with a recent study by Rees and Lummerzheim (1989) that indicates that the N2 second positive emission rate is a strongly decreasing function of the characteristic energy of the precipitating flux. These calculations reveal that a 10 keV electron will undergo approximately 160 ionizing collisions, with an average energy loss per collision of 62 eV before thermalizing. The secondary electrons are created with an average energy of 42 eV. When all processes including the backscattered escape fluxes are taken into account, the average energy loss per electron-ion pair is 35 eV in good agreement with laboratory results.

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