Auroral electron fluxes and characteristic energy of precipitating electrons: comparison between the Auroral Large Imaging System and EISCAT

Details Auroral electron fluxes and characteristic energy of precipitating electrons: comparison between the Auroral Large Imaging System and EISCAT Auroral electron fluxes and characteristic energy of precipitating electrons: comparison between the Auroral Large Imaging System and EISCAT

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm33a2140s&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM33A-2140

Other

[0310] Atmospheric Composition And Structure / Airglow And Aurora, [2407] Ionosphere / Auroral Ionosphere

Scientific paper

Reconstruction techniques can be used to analyse electron density data sets from incoherent scatter radars and emissions from ground-based imaging systems. In 2008 and 2009, coordinated radar-optical observations were organised in Lapland Scandinavia using the European Incoherent Scatter Radar (EISCAT) and the Auroral Large Imaging System (ALIS). The N2+ 1NG band at 4278Å, the green and red oxygen lines OI (5577Å) and OI (6300Å) and the near-IR OI (8446Å) line are observed by the several optical stations of the ALIS network and by means of tomography-like reconstruction techniques, the 3D volume emission rates of these emissions (with respect to altitude, latitude, longitude) are reconstructed. Inversions of the volume emission rate of N2+ and of the electron densities measured by EISCAT, using a Monte Carlo electron transport code and a few assumptions (neutral atmosphere, reaction rates), allow to derive the energy spectra of the precipitating auroral electrons. The fluxes and characteristic energy of precipitating electrons provided by both inversions are compared: the fluctuations seen of around 1 keV point to local influences such as the neutral atmosphere or the ionospheric composition. The influence of these parameters, as well as uncertainties, is discussed. Possible correlations between the characteristic energy of precipitating auroral electrons and other parameters such as auroral line intensity ratios are explored.

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