HR: 1340h
AN: SH33A-1191    [Abstracts]
TI: GEOTAIL Observation of Interplanetary Shock-Magnetic Hole Interaction on 25 September 2001: An overview
AU: * Terasawa, T
EM: terasawa@eps.s.u-tokyo.ac.jp
AF: Dept. Earth and Planetary Science, Univ. Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033 Japan
AU: Oka, M
AF: Dept. Earth and Planetary Science, Univ. Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033 Japan
AU: Nakata, K
AF: Dept. Earth and Planetary Science, Univ. Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033 Japan
AU: Tanaka, Y
AF: Dept. Earth and Planetary Science, Univ. Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033 Japan
AU: Saito, Y
AF: ISAS/JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Mukai, T
AF: ISAS/JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Kasaba, Y
AF: ISAS/JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Hayakawa, H
AF: ISAS/JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Matsuoka, A
AF: ISAS/JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Tsuruda, K
AF: ISAS/JAXA, 3-1-1 Yoshinodai, Sagamihara, 229-8510 Japan
AU: Ishisaka, K
AF: Electronics and Informatics, Toyama Prefectural Univ., Kurokawa, Kosugi-machi, 939-0938 Japan
AU: Kojima, H
AF: RISH, Kyoto University, Gokasho, Uji, 611-0011 Japan
AU: Matsumoto, H
AF: RISH, Kyoto University, Gokasho, Uji, 611-0011 Japan
AU: Keika, K
AF: Dept. Geophys., Kyoto Univ., Kitashirakawa, Sakyo-ku, Kyoto, 606-8502 Japan
AU: Nose, M
AF: WDC Kyoto, Kyoto Univ., Kitashirakawa, Sakyo-ku, Kyoto, 606-8502 Japan
AU: McEntire, R W
AF: JHU/APL, 111000 Johns Hopkins Rd., Laurel, MD 20723 United States
AB: Magnetic holes (MHs) in the solar wind are isolated depressions in the magnitude of the interplanetary magnetic field, which have attracted recent observational and theoretical attentions. On 25 September 2001, we observed an interaction event between an interplanetary shock (IPS) and a MH using the GEOTAIL data (plasma and energetic particles, magnetic and magnetic fields, and plasma waves) as well as those from the other ISTP spacecraft (ACE and WIND). What we observed were, (1) within the MH the solar wind plasma density and temperature respectively showed a decrease and increase keeping the pressure balance condition with the dropping magnetic pressure, (2) the solar wind velocity showed a significant decrease in the region surrounding the MH, (3) the nonthermal ions were trapped within the MH structure, and (4) in the MH there were enhancement of magnetic turbulence in the frequency range of 0.1-8 Hz, while no obvious enhancement was seen in the frequency range above $\sim$10 Hz. We will discuss physical implications of these observations. In addition, we are trying to deduce the evolution history of the MH-IPS system from the multi-satellite data.
DE: 7835 Magnetic reconnection
DE: 2109 Discontinuities
DE: 2134 Interplanetary magnetic fields
DE: 2139 Interplanetary shocks
DE: 2149 MHD waves and turbulence
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting