HR: 1340h
AN: P33C-0259 [Abstracts]
TI: Indirect evidence for a neutral hydrogen cloud around Titan
AU: * Szego, K
EM: szego@rmki.kfki.hu
AF: KFKI Res. Inst. for Particle and Nuclear Physics, 29-33 Konkoly Thege, Budapest, 1121
Hungary
AU: Bebesi, Z
EM: bzsofi@rmki.kfki.hu
AF: KFKI Res. Inst. for Particle and Nuclear Physics, 29-33 Konkoly Thege, Budapest, 1121
Hungary
AU: Erdos, G
EM: erdos@rmki.kfki.hu
AF: KFKI Res. Inst. for Particle and Nuclear Physics, 29-33 Konkoly Thege, Budapest, 1121
Hungary
AU: Foldy, L
EM: foldy@rmki.kfki.hu
AF: KFKI Res. Inst. for Particle and Nuclear Physics, 29-33 Konkoly Thege, Budapest, 1121
Hungary
AU: Crary, F
EM: fcrary@swri.edu
AF: Southwest Research Institute, 6220 Culdebra Road, San Antonio, TX 78228-0510
United States
AU: Young, D T
EM: dyoung@swri.edu
AF: Southwest Research Institute, 6220 Culdebra Road, San Antonio, TX 78228-0510
United States
AU: Coates, A J
EM: ajc@mssl.ucl.ac.uk
AF: Mullard Space Science Laboratory, Surrey, Holmbury St.Mary, RH5 6NT
United Kingdom
AU: Rymer, A
EM: amr@mssl.ucl.ac.uk
AF: Mullard Space Science Laboratory, Surrey, Holmbury St.Mary, RH5 6NT
United Kingdom
AU: Hartle, R E
EM: Robert.E.Hartle@nasa.gov
AF: Goddard Space Flight Center, Greenbelt, Greenbelt, MD 20771
United States
AU: Sittler, E C
EM: Edward.C.Sittler@nasa.gov
AF: Goddard Space Flight Center, Greenbelt, Greenbelt, MD 20771
United States
AU: Berthelier, J J
EM: jean_jacques.berthelier@cetp.ipsl.fr
AF: Centre d'étude des Environnements Terrestre et Planetaires, 4 Av Neptune, St Maur,
94107
France
AU: Bouhram, M
EM: mehdi.bouhram@cetp.ipsl.fr
AF: Centre d'étude des Environnements Terrestre et Planetaires, 4 Av Neptune, St Maur,
94107
France
AU: Thomsen, M F
EM: mthomsen@lanl.gov
AF: Los Alamos National Laboratory, Los Alamos, Los Alamos, NM 87545
United States
AU: Eviatar, A
EM: arkee1@daphne.tau.ac.il
AF: Tel Aviv University, Tel Aviv, Tel Aviv, 2341
Israel
AB:
During the TA flyby inbound, between 15 R-Titan and 4 R-Titan, the Cassini Plasma Spectrometer (CAPS) detected ions which
were very likely pick-up ions. These ions
-always arrived from a direction perpendicular to the local magnetic field,
-had a narrow spectrum in the count-energy plots,
-always appeared in pairs with energy ratio 2,
-were identified as m/q=1 and m/q=2 ions when simultaneous time of flight data were available,
-were observed during 11 consecutive actuator sweeps,
-in most of the cases the velocities were about twice of the corotating plasma velocity.
If they were pickup ions, they could not originate from Titan because they were observed at much larger distances than those
of what ions escaping from the moon could cover. Another option is that they arrived from a local source, possibly from a
local neutral cloud.
In this study we analyse first whether it can be substantiated that the ion population described above were pickup ions, and
we also investigate all the other encounters to clarify whether such pickup population are a permanent feature of the plasma
environment of Titan.
DE: 2756 Planetary magnetospheres (5443, 5737, 6033)
DE: 6281 Titan
SC: Planetary Sciences [P]
MN: Fall Meeting 2005