HR: 1340h
AN: P43A-0963    [Abstracts]
TI: Electron energetics of Titan's ionosphere
AU: * Robertson, I P
EM: robertin@ku.edu
AF: University of Kansas, Department of Physics & Astronomy, Malott Hall, 1251 Wescoe Hall Dr., Room 1082 , Lawrence, KS 66045-7582 United States
AU: Cravens, T E
EM: cravens@ku.edu
AF: University of Kansas, Department of Physics & Astronomy, Malott Hall, 1251 Wescoe Hall Dr., Room 1082 , Lawrence, KS 66045-7582 United States
AU: Coates, A
EM: ajc@mssl.ucl.ac.uk
AF: University College London, Mullard Space Science Laboratory, Holmbury St Mary, Dorking, RH5 6NT United Kingdom
AU: Wahlund, J
EM: jwe@irfu.se
AF: Swedish Institute of Space Physics, Uppsala Division, Box 537, Uppsala, SE-751 21 Sweden
AU: Young, D
EM: dyoung@swri.edu
AF: Southwest Research Institute, 6220 Culebra Road, P.O. Drawer 28510, San Antonio, TX 78228-0510 United States
AU: Rowland, W
EM: wfr2k@hotmail.com
AF: University of Kansas, Department of Physics & Astronomy, Malott Hall, 1251 Wescoe Hall Dr., Room 1082 , Lawrence, KS 66045-7582 United States
AU: Waite, J H
EM: hunterw@umich.edu
AF: University of Michigan, Dept. of Atmospheric, Oceanic, and Space Sciences, Ann Arbor, MI 48109-2143 United States
AU: Nagy, A
EM: anagy@engin.umich.edu
AF: University of Michigan, Dept. of Atmospheric, Oceanic, and Space Sciences, Ann Arbor, MI 48109-2143 United States
AU: Ma, Y
EM: yingjuan@umich.edu
AF: University of Michigan, Dept. of Atmospheric, Oceanic, and Space Sciences, Ann Arbor, MI 48109-2143 United States
AB: During encounters with Titan in situ measurements were made of Titan's atmosphere and ionosphere by the Ion and Neutral Mass Spectrometer (INMS) instrument on the Cassini Orbiter. The electron density and temperature in the ionosphere were measured with the Langmuir probe on the Cassini Radio and Plasma Wave Experiment (RPWS) and supra-thermal electron fluxes were measured by the CAPS instrument. Both solar and magnetospheric inputs are important for the electron energetics of Titan's atmosphere. The magnetospheric inputs are especially important on Titan's nightside. We varied several inputs into our model of the electron energetics in order to obtain agreement between observed and modeled electron temperatures. We used magnetic field lines from a global MHD model for constraining our heat conduction.
DE: 5405 Atmospheres (0343, 1060)
DE: 5410 Composition (1060, 3672)
DE: 5418 Heat flow
SC: Planetary Sciences [P]
MN: Fall Meeting 2005