Mathematics – Logic
Scientific paper
Apr 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jgra..11304305k&link_type=abstract
Journal of Geophysical Research, Volume 113, Issue A4, CiteID A04305
Mathematics
Logic
3
Atmospheric Composition And Structure: Airglow And Aurora, Ionosphere: Particle Precipitation, Atmospheric Composition And Structure: General Or Miscellaneous, Ionosphere: General Or Miscellaneous
Scientific paper
The launch of the Defense Meteorological Satellite Program (DMSP) satellite F16 in 2003 provided the first opportunity to analyze extensive sets of high-quality coincident auroral particle and FUV data obtained by the onboard sensors Special Sensor Ultraviolet Spectrographic Imager (SSUSI) and Special Sensor Auroral Particle Sensor (SSJ/5). Features of interest are Ly α (121.6 nm), Lyman-Birge-Hopfield short (LBHS, the SSUSI 140-150 nm channel), and Lyman-Birge-Hopfield long (LBHL, 165-180 nm). We report on comparisons of column emission rates (CERs) by deriving simulated SSUSI values using SSJ/5 electron and ion (treated as proton) spectra. Field-line tracing is performed to determine the locations of coincidences. CERs are obtained by integrating the products of particle spectra and monoenergetic emission yields. A technique is reported for deriving these yields from nonmonoenergetic CERs obtained by our particle transport model. SSJ/5 ion spectra are extrapolated above 30 keV using a statistical representation based on Polar Orbiting Environmental Satellites particle data. Key quantities of interest are ratios of SSUSI to SSJ/5-based CERs (S-S ratios) and corresponding ratios of proton-produced to total emission (unity for Ly α and from 0 to 1 for LBHS and LBHL). SSJ/5-based CERs are used to derive the latter ratios. Median ratio values are determined in order to reduce the error budget to primarily calibration and model errors. The median LBH S-S ratios increase by a factor of ~2.5 from electron to proton aurora and support significantly higher proton LBH emission efficiencies (3 times the electron efficiencies) assuming reported calibration uncertainties. This calls for significant increases in proton and/or H-atom LBH cross sections. In turn, FUV auroral remote-sensing algorithms must explicitly address both electron and proton aurora.
Evans Silvan D.
Hecht James H.
Knight H. K.
Morrison Douglas
Paxton Larry J.
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