Derivation of Auroral Conductances from IMAGE FUV

Details Derivation of Auroral Conductances from IMAGE FUV Derivation of Auroral Conductances from IMAGE FUV

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sa41a10i&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SA41A-10

Physics

0310 Airglow And Aurora, 0358 Thermosphere--Energy Deposition

Scientific paper

Auroral emissions are observed in 3 separate Far-Ultraviolet (FUV) wavelength regimes by IMAGE. The Wideband Imaging Camera (WIC) is sensitive mainly to N2 LBH and N I emissions in the 140-190-nm range, while the Spectrographic Imager (SI) spectrally separates the OI 135.6-nm emission and Doppler shifted hydrogen emissions of the proton aurora at 121.8 nm. The brightness of the N2 LBH and OI 135.6-nm emissions depend in part on the spectrum and total energy flux of incoming electrons, and on the height-density profile of the respective species, and O2. Due mainly to these atmospheric factors, the ratio of the N2 and OI emissions depends strongly on the characteristic energy of precipitating electrons which, once estimated, can in turn be used to calculate the total energy flux. The proton aurora generates secondary electrons, which excite additional emissions of N2 and OI. It is not possible to absolutely determine either the total proton energy flux or the characteristic proton energy () with a single proton imaging channel. However, the proton-induced N2 and OI emissions depend mainly on the total proton energy flux, so reasonable estimates of can be used in the calculation of proton energy input. Ground-based or in-situ observations of proton energies can help in this determination. With accurate corrections for N2 and OI airglow emissions, and formulae such as those provided by Robinson et al. [1987], IMAGE FUV can provide global maps of height-integrated conductivity (conductance) in the auroral oval. It is also possible to examine the degree to which the proton aurora contributes to enhanced conductance on a global scale. The promise of providing these conductances using IMAGE's real-time capabilities will be discussed. Robinson, R. M., R. R. Vondrak, K. Miller, T. Dabbs, and D. Hardy, On Calculating Ionospheric Conductances from the Flux and Energy of Precipitating Electrons, J. Geophys. Res., 92, 2566, 1987.

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