Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm41a1834l&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SM41A-1834
Physics
[0310] Atmospheric Composition And Structure / Airglow And Aurora, [2704] Magnetospheric Physics / Auroral Phenomena, [2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions
Scientific paper
This study presents the results of a comparison study between the FUV auroral observations and the electron spectrum measured simultaneously on the same spacecraft. The FUV auroral observations were made from the dual band FUV imaging spectrograph, FIMS, on STSAT-1 operated at an altitude of 685 km in a sun-synchronous orbit. The bandwidths of FIMS are 90.0-115.0 nm for the S-band with a 0.2 nm spectral resolution and 134.0-171.5 nm for the L-band with a 0.3 nm spectral resolution. The electron spectrum was obtained with an Electrostatic Analyzer (ESA) for the electron energy from 100 eV to 20 keV and a Solid State Telescope (SST) for the energy from 170 keV to 350 keV. We divided the polar region into five sub-regions: (a) dayside diffuse zone (part of the dayside radiation belt), (b) dayside auroral zone, (c) polar cap, (d) nightside auroral zone, and (e) nightside diffuse zone (part of the nightside radiation belt). OI 98.9 nm, HI & OI 102.6 nm, and NII 108.5 nm are the most visible lines in the S-band regardless of the regions though their ratios clearly depend on the electron energy spectrum. For example, NII 108.5 nm becomes dominant in the region where high energy electrons precipitate. In the L-band, OI 135.6 nm, NI 149.3 nm, and N2 Lyman-Birge-Hopfield (LBH) lines are prominent regardless of the regions. The intensity ratio of the long LBH to the short LBH is seen higher in the region where the electron spectrum is harder. We will discuss general characteristics of the FUV spectra in the above mentioned sub-regions compared with the corresponding electron spectra.
Lee Chaohong
Min Kyoung-Wook
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