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

[PPS01-P07] Reconsideration for causalities of occurrence features of Jupiter's Io-related radio emission

*三澤 浩昭¹、熊本 篤志²、安田 陸人¹ (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.東北大学大学院理学研究科　地球物理学専攻)

キーワード：木星、イオ、オーロラ電波、レイトレーシング

The magneto-ionic wave mode and generation processes of Jupiter's auroral decametric radio emission have been long years subjects required for verification. We have investigated the subjects particularly for Io-related component (Io-DAM) based on numerical calculations using several kinds of magnetic field and plasma density models, however, the questions have not been resolved yet: a hypothesis of some special energy transportations along the magnetic field line connecting to Io is required to explain the observed occurrence probability and polarization of Io-DAM. Recently Jupiter's new magnetic field model 'JRM09' was proposed based on the magnetic field observations near Jupiter conducted by the 'Juno' Jupiuter explorer (Connerney+, GRL, 2018). We have tried to make a 3D ray-tracing analysis for Io-DAM adopting the JRM09 model. The preliminary analyses show that R-X mode waves are preferable as Io-DAM and the JRM09 gives more natural explanations for the origin of Io-DAM than the previous magnetic field models, though there still remain some questions on occurrence restriction of Io-DAM (e.g. 'generation source of the Io-C emissions'). In the presentation, we will introduce remaining questions on observed Io-DAM and the trial of the ray-tracing analysis including polarization explanation.