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

[PPS01-01] Circulation of plasma in the Jupiter's inner magnetosphere revealed from time variation in radial profile of plasma temperature and density obtained by Hisaki/EXCEED observation

*疋田 伶奈¹、吉岡 和夫²、土屋 史紀³、鍵谷 将人³、村上 豪⁴、木村 智樹⁵、山崎 敦⁴、吉川 一朗² (1.東京大学大学院 理学系研究科 地球惑星科学専攻、2.東京大学大学院　新領域創成科学研究科　複雑理工学専攻、3.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、4.宇宙航空研究開発機構 宇宙科学研究所、5.東北大学　学際科学フロンティア研究所)

The satellite Io, which has many volcanoes and is located at 5.9 R_J from the center of Jupiter, is a powerful plasma source in the magnetosphere. The resulting specificity of the Jupiter's magnetosphere is the magnitude of energy that circulates internally. Previous researches, using data obtained by Voyager and Cassini spacecraft and chemical models complementarily, showed that the pickup energy of heavy ions originating from volcanoes on Io and the energy of hot electrons are converted into radiation reaching ~3 TW. However, the origins of hot electrons, that is, heating and/or transport mechanisms are still unrevealed. Therefore, in this research, we focus on the response to the change in the amount of plasma supplied to the magnetosphere and explore the above problem. In this study, the radial distributions of plasma density and temperature were derived from the intensities of emission lines in the extreme ultraviolet range obtained by Hisaki satellite. In this presentation, we will show the results using data obtained from December 2014 to May 2015. The activation of volcanoes on Io in early January 2015 was confirmed by ground-based infrared observations.