JpGU-AGU Joint Meeting 2020

講演情報

[E] 口頭発表

セッション記号 P (宇宙惑星科学) » P-CG 宇宙惑星科学複合領域・一般

[P-CG25] 惑星大気圏・電磁圏

コンビーナ:関 華奈子(東京大学大学院理学系研究科)、今村 剛(東京大学大学院 新領域創成科学研究科)、前澤 裕之(大阪府立大学大学院理学系研究科物理科学科)、寺田 直樹(東北大学大学院理学研究科)

[PCG25-10] 磁気圏電子とエンケラドス衛星起源H2Oとの弾性衝突の数値計算

*田所 裕康1加藤 雄人2 (1.武蔵野大学、2.東北大学大学院)

キーワード:弾性衝突、エンケラドス、土星

Saturn’s inner magnetosphere is dominated by water group neutrals originated from Enceladus. The water group neutrals (H2O, OH, and O) play the dominant role in loss of energetic plasmas [e.g., Paranicas et al., 2007; Sittler et al., 2008]. The observations of injected plasmas in the inner magnetosphere suggest that these particles do not survive very long time due to the neutral cloud originated from Enceladus [e.g., Paranicas et al., 2007; 2008]. Thus, the previous studies suggested that the neutrals contribute to loss processes of plasma in the inner magnetosphere. However, little has been reported on a quantitative study of the electron loss process due to electron-neutral collisions.

Tadokoro et al., [2014] examined the time variations of equatorial electron pitch angle distribution and electrons within loss cone through 1keV electron pitch angle scattering due to elastic collisions around Enceladus, conducting one dimensional test particle simulation. The result showed that the electrons of 11.4 % are lost in ~380 sec. This time corresponds to the time scale of the co-rotation of the flux tube passing through the region of the dense H2O in the vicinity of Enceladus. Assuming the uniform azimuth H2O density structure in the Enceladus torus, they estimated the electron loss rate of 33% during one co-rotation.
We show the energy dependent electron (500 eV – 50 keV) loss rates through pitch angle scattering due to elastic collisions. We show the comparison of the loss rates between the high (in the vicinity of Enceladus) and low (in the Enceladus torus) H2O density regions. The collision is solved by a Monte-Carlo method. The cross section is based on experimental data. We show the calculation errors by making 10 times calculations. We also estimate the auroral brightness by using calculated electrons.