HR: 0800h
AN: SA31A-0346 [Abstracts]
TI: Neutral Atom Emission in the Direction of the High-Latitude Magnetopause for Northward IMF:
Simultaneous Observations From IMAGE Spacecraft and SuperDARN Radar
AU: * Taguchi, S
EM: taguchi@ice.uec.ac.jp
AF: Univ. of Electro-Communications, Chofugaoka, Chofu, 182-8585
Japan
AU: Hosokawa, K
EM: hosokawa@ice.uec.ac.jp
AF: Univ. of Electro-Communications, Chofugaoka, Chofu, 182-8585
Japan
AU: Murata, Y
EM: ymurata@ice.uec.ac.jp
AF: Univ. of Electro-Communications, Chofugaoka, Chofu, 182-8585
Japan
AU: Nakao, A
EM: nakao@ice.uec.ac.jp
AF: Univ. of Electro-Communications, Chofugaoka, Chofu, 182-8585
Japan
AU: Collier, M R
EM: michael.r.collier@nasa.gov
AF: NASA/GSFC, Code 612.2, Greenbelt, MD 20771
United States
AU: Moore, T E
EM: thomas.e.moore@nasa.gov
AF: NASA/GSFC, Code 612.2, Greenbelt, MD 20771
United States
AU: Yamazaki, A
EM: yamazaki@pparc.geophys.tohoku.ac.jp
AF: Tohoku Univ., Aoba, Sendai, 980-8578
Japan
AU: Sato, N
EM: nsato@nipr.ac.jp
AF: NIPR, Itabashi, Tokyo, 173-8515
Japan
AU: Yukimatu, A S
EM: sessai@nipr.ac.jp
AF: NIPR, Itabashi, Tokyo, 173-8515
Japan
AB:
During a northward interplanetary magnetic field on 27 March 2001, the Low Energy Neutral Atom (LENA) imager on the IMAGE
spacecraft in the magnetosphere observed an enhanced emission in the direction of the very high-latitude magnetopause.
Simultaneous observations from IMAGE/LENA and SuperDARN radar show that the LENA emission appears concurrently with the
enhancement of the sunward flow of the reverse convection in the ionosphere. The field line mapping from the magnetosphere
to the ionosphere suggests that the source ions for the LENA emission are in the sunward flow region. Although the direction
of the emission is relatively stable, its direction gradually changes so that the emission may shift poleward and then
return equatorward. From these observations, we suggest that LENA can monitor the ion entry caused by cusp reconnection and
that the reconnection site moves on a time scale of several minutes. Such motion is discussed in terms of the solar wind
variations.
DE: 2455 Particle precipitation
DE: 2463 Plasma convection (2760)
DE: 2706 Cusp
DE: 2723 Magnetic reconnection (7526, 7835)
SC: SPA-Aeronomy [SA]
MN: Fall Meeting 2005