HR: 1340h
AN: SM43B-1230    [Abstracts]
TI: Testing Auroral Far Ultraviolet (FUV) Remote Sensing Techniques Using Coincident FUV and Particle Data From the DMSP F16 Satellite
AU: * Knight, H K
EM: knight@cpi.com
AF: Computational Physics, Inc, 8001 Braddock Rd Suite 210, Springfield, VA 22151 United States
AU: Strickland, D J
EM: dstrick@cpi.com
AF: Computational Physics, Inc, 8001 Braddock Rd Suite 210, Springfield, VA 22151 United States
AU: Kochenash, A J
EM: ajk@cpi.com
AF: Computational Physics, Inc, 8001 Braddock Rd Suite 210, Springfield, VA 22151 United States
AU: Hecht, J H
EM: james.hecht@aero.org
AF: The Aerospace Corp, MS M2-259 PO Box 92957, Los Angeles, CA 90009 United States
AU: Morrison, D
EM: danny.Morrison@jhuapl.edu
AF: Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Zhang, Y
EM: yongliang.zhang@jhuapl.edu
AF: Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Paxton, L J
EM: larry.paxton@jhuapl.edu
AF: Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Burke, W J
EM: william.burke2@hanscom.af.mil
AF: Air Force Research Lab, AFRL/VSBXP 29 Randolph Rd, Hanscom AFB, MA 01731 United States
AU: Rich, F J
EM: frederick.rich@hanscom.af.mil
AF: Air Force Research Lab, AFRL/VSBXP 29 Randolph Rd, Hanscom AFB, MA 01731 United States
AB: A number of investigators over the years have used far ultraviolet (FUV) observations of the aurora to infer particle precipitation characteristics (energy flux Q [in mW m^-2] and either a characteristic energy E_o (in keV) or an average energy E_avg). With the launch of the AF DMSP F16 satellite in November 2003, we have an opportunity to evaluate this technique (auroral FUV remote sensing) using FUV observations from the SSUSI sensor in coincidence with particle observations from the SSJ/5 sensor (both on F16). SSUSI measures FUV emission in five spectral channels of which three are addressed here: HI Ly α (121.6 nm), LBH_S and LBH_L. The latter two channels are dominated by N₂ LBH emission with approximate spectral ranges of 140-150 nm and 165-180 nm, respectively. SSJ/5 measures the spectra of electrons and protons from 30 eV to 30 keV from which E_avg and Q are derived for both types of precipitation. The SSUSI-based E_avg and Q to be compared with those from SSJ/5 correspond to a SSUSI look angle determined from tracing magnetic fieldlines at the satellite down to 120 km. We assume that the peak of volume emission corresponding to SSJ/5 measurements is at 120 km although the resulting look angle is not sensitive to the nominal range of peak altitudes from, say, 150 to 100 km. Basic results to be presented are coincident E_avg and Q from the two sensors. The emphasis in this work will be on statistical results to be presented in the form of the LBH_L emission yield (kiloRayleighs/unit Q) versus the [proton Q/total Q] ratio where all Q values refer to those measured by SSJ/5. Among findings to date is an increase in emission efficiency for proton/H-atom aurora compared to electron aurora that complicates auroral FUV remote sensing in the absence of independent information on Eavg for protons.
DE: 0310 Airglow and aurora
DE: 2455 Particle precipitation
DE: 2704 Auroral phenomena (2407)
DE: 2716 Energetic particles: precipitating
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005