HR: 0800h
AN: SM31A-1219    [Abstracts]
TI: Pi2 Observations by Cluster and Ground Stations
AU: Takada, T
EM: taku.takada@oeaw.ac.at
AF: Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, 8042 Austria
AU: Volwerk, M
EM: martin.volwerk@oeaw.ac.at
AF: Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, 8042 Austria
AU: Volwerk, M
EM: martin.volwerk@oeaw.ac.at
AF: Max Planck Institute for Extraterrestrial Physics, Postfach 1312, Garching, 85741 Germany
AU: * Nakamura, R
EM: rumi.nakamura@oeaw.ac.at
AF: Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, 8042 Austria
AU: Baumjohann, W
EM: baumjohann@oeaw.ac.at
AF: Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, 8042 Austria
AU: Zhang, T L
EM: tielong.zhang@oeaw.ac.at
AF: Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, Graz, 8042 Austria
AU: Uozumi, T
EM: uozumi@serc.kyushu-u.ac.jp
AF: Space Environment Research Center, Dept. of Earth and Planetary Sciences, Kyushu University 33, 6-10-1 Hakozaki, Fukuoka, 812-8581 Japan
AU: Glassmeier, K
EM: kh.glassmeier@tu-bs.de
AF: Institute for Geophysics and Extraterrestrial Physics, TU Braunschweig, Mendelssohnstr. 3, Braunschweig, 38106 Germany
AU: Klecker, B
EM: berndt.klecker@mpe.mpg.de
AF: Max Planck Institute for Extraterrestrial Physics, Postfach 1312, Garching, 85741 Germany
AU: Balogh, A
EM: a.balogh@imperial.ac.uk
AF: Space and Atmospheric Physics Group, Dept. of Physics, H/6M67A, Huxley Building Imperial College, London, SW7 2AZ United Kingdom
AU: R\`eme, H
EM: reme@cesr.fr
AF: CESR, BP 4346, Toulouse, 31028 France
AB: We will present case studies of conjugate Pi2 observations by Cluster in the magnetotail ($\sim 19 R_{\rm E}$) and ground stations from the 210 meridian magnetometer chain. Comparing the magnetic field data for these events we find similar waveforms at Cluster and on the ground. Using the spatial separation of the Cluster spacecraft we can determine the propagation direction of the waves. The waves observed by Cluster are travelling tailward with velocities up to $\sim 800$ km/s. When possible, we will use the time difference between the observation on the ground and by Cluster to get an estimate of where these waves are generated.
DE: 2744 Magnetotail
DE: 2752 MHD waves and instabilities
DE: 2772 Plasma waves and instabilities
DE: 2788 Storms and substorms
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting