日本地球惑星科学連合2019年大会

講演情報

[E] ポスター発表

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-EM10] Multi-scale Coupling in the Magnetosphere-Ionosphere-Thermosphere System

2019年5月27日(月) 13:45 〜 15:15 ポスター会場 (幕張メッセ国際展示場 8ホール)

コンビーナ:Yue Deng(University of Texas at Arlington)、Toshi Nishimura(Boston University)、Liu Huixin(九州大学理学研究院地球惑星科学専攻 九州大学宙空環境研究センター)、Yanshi Huang(Harbin Institute of Technology, Shenzhen)

[PEM10-P04] A long-lasting auroral bright spot around magnetic north pole: Is it the evidence of stable magnetic reconnection?

*Qing-He Zhang1Guo-Cheng Shen1Yong-Liang Zhang2Kjellmar Oksavik3Michael Lockwood4Zan-Yang Xing1Yu-Zhang Ma1 (1.Institute of Space Sciences, Shandong University, Weihai, China、2.The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, USA、3.Birkeland Centre for Space Science, University of Bergen, Bergen, Norway、4.Department of Meteorology, University of Reading, Earley Gate, Post Office Box 243, RG6 6BB, UK.)

キーワード:Auroral bright spot, Magnetosphere-ionosphere coupling, High-latitude lobe magnetic reconnection, Stable reconnection

An intense and large auroral bright spot appears around the magnetic north pole observed by the Special Sensor Ultraviolet Spectrographic Imager (SSUSI) on board four different Defense Meteorological Satellite Program (DMSP) satellites during long time northward IMF conditions. The bright spot is even brighter than aurora in the auroral oval which is about 5-10° magnetic latitude equatorward of the bright spot. The bright spot is lasting about 8 hours, and sometimes appears as a cyclone-shape with a clockwise rotation. The DMSP in situ plasma observations suggest that the bright spot is clear associated with electron invert-V acceleration with 10s keV energy electron precipitations around the center regions and 1s keV energy electron precipitations around the egde regions. There are also strong flow shears between the two sides of the bright spot: strong sunward flows on the duskside and antisunward flows on the dawnside. These types of plasma should come from the high-latitude lobe region of the magnetotail due to the high-latitude lobe magnetic reconnections. Is it the evidence of stable lobe reconnection during long time northward IMF conditions? The detail and further analysis should be pursued in the following studies.