日本地球惑星科学連合2015年大会

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セッション記号 P (宇宙惑星科学) » P-EM 太陽地球系科学・宇宙電磁気学・宇宙環境

[P-EM28] 磁気圏-電離圏ダイナミクス

2015年5月27日(水) 18:15 〜 19:30 コンベンションホール (2F)

コンビーナ:*三好 由純(名古屋大学太陽地球環境研究所)、長谷川 洋(宇宙航空研究開発機構宇宙科学研究所)、中野 慎也(情報・システム研究機構 統計数理研究所)、田中 良昌(国立極地研究所)、堀 智昭(名古屋大学太陽地球環境研究所 ジオスペース研究センター)

18:15 〜 19:30

[PEM28-P12] Geotailで観測された昼側磁気圏境界面での磁気リコネクションⅠ

*吉田 和史1小田切 修一1長井 嗣信2 (1.東工大・地惑、2.東京工業大学)

キーワード:磁気圏, 磁気リコネクション

On 06 July 2013, Geotail observed the dayside magnetopause reconnection for a long time period. In the period 0000-0800 UT on 06 July 2013, the solar wind has an almost constant speed of 350 km/s and the Interplanetary Magnetic Field (IMF) is almost southward, having a value of (0.0, +4.5, -12.0 nT). Geotail traveled from the magnetosheath to the magnetosphere. The Geotail position is (Xgsm, Ygsm, Zgsm) = (9.72, -2.23, -0.49 Re) at 0400 UT and (8.91, 0.87, -1.73) at 0600 UT, respectively. Geotail stays in the vicinity of the magnetopause, almost in the front magnetosphere. Reconnection jets with a speed of 200 km/s are observed near the reversal of the magnetic field. The reconnection jets flow northward, indicating that the reconnection site is located south of the Geotail position. There are two cases in the magnetic field variations. In most cases, the Bz magnetic field component is dominant and the field reverses from southward to northward in the crossing into the magnetosphere, and the reconnection jets are almost field-aligned. However, the magnetic field becomes almost perpendicular to the north-south direction, and the positive By magnetic field component is dominant. The reconnection jets are convection flows. In this study, the magnetic field topology and its relationship to the jets are investigated.