日本地球惑星科学連合2016年大会

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セッション記号 P (宇宙惑星科学) » P-PS 惑星科学

[P-PS01] Outer Solar System Exploration Today, and Tomorrow

2016年5月22日(日) 13:45 〜 15:05 A02 (アパホテル&リゾート 東京ベイ幕張)

コンビーナ:*木村 淳(東京工業大学地球生命研究所)、藤本 正樹(宇宙航空研究開発機構・宇宙科学研究本部)、笠羽 康正(東北大学大学院 理学研究科 地球物理学専攻)、佐々木 晶(大阪大学大学院理学研究科宇宙地球科学専攻)、谷川 享行(産業医科大学医学部)、関根 康人(東京大学大学院理学系研究科地球惑星科学専攻)、Sayanagi Kunio(Atmospheric and Planetary Sciences Department, Hampton University)、Vance Steven(Jet Propulsion Laboratory, Caltech)、座長:三澤 浩昭(東北大学大学院理学研究科惑星プラズマ・大気研究センター)、吉岡 和夫(東京大学大学院理学系研究科地球惑星科学専攻)

14:35 〜 14:50

[PPS01-15] Io's volcanic influence on the Jovian magnetosphere: HISAKI observation

*土屋 史紀1吉岡 和夫2木村 智樹3村上 豪4米田 瑞生5古賀 亮一1鍵谷 将人1野澤 宏大6垰 千尋7三澤 浩昭1坂野井 健1笠羽 康正8山崎 敦4吉川 一朗9 (1.東北大学大学院理学研究科惑星プラズマ・大気研究センター、2.東京大学大学院理学研究科、3.理研、4.宇宙科学研究所、5.キーペンハウアー太陽物理学研究所、6.鹿児島高専、7.情報通信研究機構、8.東北大学大学院理学研究科、9.東京大学大学院新領域創成科学研究科)

The satellite Io which has many active volcanos supplies volcanic gases to the Jovian magnetosphere with a typical rate of 1 ton/sec and has is a primary source of plasmas in the magnetosphere. Change in the volcanic activity would cause change in plasma supply rate to the magnetosphere and could affect structure of the magnetosphere and dynamics occurring in it. However, responses of the magnetosphere to the plasma supply rate change is still not fully understood. The extreme ultraviolet (EUV) spectroscope, EXCEED, onboard the HISAKI satellite made observations of Io plasma torus and Jovian northern aurora from the end of Nov. 2014 to middle of May 2015 continuously. On middle of Jan. 2015, HISAKI detected gradual increase in intensity of S+ emission lines and decrease of S3+ ones in the plasma torus. The S+ intensity showed a maximum around the end of Feb. and S2+ and S3+ intensities also showed maxima subsequently. Simultaneous ground based observation of the sodium nebula showed increase of the emission intensity from the middle of Jan. to Feb. These observations suggest that the volcanic activity enhancement started at the middle of Jan. and increase neutral atom and ion densities in the Io torus. Change in radial structure of the plasma torus was also detected. The intensity of S+ ion began to increase around the orbit of Io (6 Jovian radii). The brightened region propagated outward and reached at 8.5 Jovian radii from Jupiter at the beginning of Feb. Further one month later, HISAKI found unusual activity of Jovian EUV aurora intensity. It began at the beginning of Mar. and continued for 1 month. The enhancement of the aurora activity may be caused by the enhanced loading of heavy ion plasma into the middle magnetosphere.