HR: 10:30h
AN: SA32A-01    [Abstracts]
TI: Integrated Solar Irradiance from 1-45 nm (Qeuv) as Determined from the GUVI instrument on TIMED
AU: * Morrison, D
EM: daniel.morrison@jhuapl.edu
AF: Johns Hopkins Applied Physics Lab, 11100 Johns Hopkins Rd., Laurel, MD 20723 United States
AU: Wolven, B
EM: brian.wolven@jhuapl.edu
AF: Johns Hopkins Applied Physics Lab, 11100 Johns Hopkins Rd., Laurel, MD 20723 United States
AU: Paxton, L
EM: larry.paxton@jhuapl.edu
AF: Johns Hopkins Applied Physics Lab, 11100 Johns Hopkins Rd., Laurel, MD 20723 United States
AB: The N₂ LBH emission produced by photoelectron impact is one of the core emissions used for remote sensing of the thermosphere. This emission forms the basis for a proxy of EUV solar flux (< 45 nm, Qeuv) when used with OI 135.6 nm signals to derive O/N₂ column ratios in the thermosphere (Strickland et al. [1995]). The LBH cross section used comes from Ajello and Shemansky [1985]. Recently, experimenters have argued for an increase in this cross section by as much as a factor of 1.6 (Budzien et al. [1994] and Eastes [2000]). When the increased cross section is used the Qeuv estimated from GUVI data is considerably smaller than the solar irradiance measurements in this bandpass as measured by the SEE instrument, also flying on TIMED. This has led some to question the accuracy of the SEE values. We will show that using the established N₂ LBH emission cross sections we can derive Qeuv measurements from the GUVI data that are very consistent with the SEE irradiance measurements, simply by relaxing an assumption that has normally been used to determine O/N₂ ratios and Qeuv from the GUVI data.
DE: 0310 Airglow and aurora
DE: 0343 Planetary atmospheres (5405, 5407, 5409, 5704, 5705, 5707)
DE: 0358 Thermosphere--energy deposition
DE: 0394 Instruments and techniques
DE: 7538 Solar irradiance
SC: SPA-Aeronomy [SA]
MN: 2005 Joint Assembly