HR: 12:05h
AN: SA31B-07    [PDF]
TI: Analysis of the Energy Input and Loss in the Thermosphere During the Auroral Events Using SABER Infrared Limb Emission and GUVI Limb Emission
AU: * Winick, J R
EM: jeremy.winick@hanscom.af.mil
AF: AFRL/Space Vehicles Directorate, 29 Randolph Rd., Hanscom AFB, Bedford, MA 01731
AU: Mlynczak, M G
AF: NASA/LARC, MS-401B, Hampton, VA 23681
AU: Wintersteiner, P P
AF: Arcon Corp., 260 Bear Hill Rd., Waltham, MA 02451
AU: Martin-Torres, F
AF: AS+M Corp., 1 Enterprise Pkwy., Hampton, VA 23666
AU: Picard, R H
AF: AFRL/Space Vehicles Directorate, 29 Randolph Rd., Hanscom AFB, Bedford, MA 01731
AU: Paxton, L
AF: JHU/APL, 11100 Johns Hopkins Rd., Laurel, MD 20723
AU: Lopez-Puertas, M
AF: Instituto de Astrofisica de Andalucia (CSIC), Apdo. 3004, Grenada, E-18080 Spain
AU: Mertens, C J
AF: NASA/LARC, MS-401B, Hampton, VA 23681
AU: Russell, J M
AF: Hampton Univ., Center for Atmospheric Sciences, Hampton, VA 23668
AU: Christensen, A
AF: Aerospace Corp., P.O. Box 92957, Los Angeles, CA 90009
AU: Gordley, L L
AF: GATS Inc., 11864 Canon Blvd., Newport News, VA 23606
AB: The SABER instrument on TIMED is continuously measuring limb radiance profiles of CO$_{2}$ $\nu$$_{3}$ (4.3-$\mu$m) and $\nu$$_{2}$ (15-$\mu$m) and NO (5.3-$\mu$m) with unprecedented sensitivity. SABER provides limb radiances up to $\sim$130km for the 15-$\mu$m channel and $\sim$140-150km (approaching 200km during strong auroral events) for the 4.3-$\mu$m channel and over 200km (to 300km during storm conditions) for the 5.3-$\mu$m channel. From the SABER infrared channels and the GUVI FUV we have a measure of the auroral energy input at high latitudes into the lower thermosphere and its transport southward and its radiative loss through NO emission. We have previously reported that during the April 2002 geomagnetic storm the 4.3-$\mu$m band nighttime emission was enhanced dramatically in the high latitude regions. The NO 5.3-$\mu$m band emission also dramatically increased but it was not limited to the auroral zone. We extend this analysis to the October 2002 and May 2003 geomagnetic storms and to more isolated (short time) but strong auroral events. We will compare the morphology and time dependence of the enhancement in the 4.3-$\mu$m and 5.3-$\mu$m channels. Examining different situations in terms of length and strength of energy input allows us to better determine the lifetime of the enhanced NO emission (and hence a clue to the NO cooling) and the contribution of excited NO from auroral chemistry versus temperature and composition changes.
DE: 0310 Airglow and aurora
DE: 0342 Middle atmosphere--energy deposition
DE: 0358 Thermosphere--energy deposition
SC: SPA - Aeronomy [SA]
MN: 2003 Fall Meeting