日本地球惑星科学連合2024年大会

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[E] 口頭発表

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-EM15] 太陽地球系結合過程の研究基盤形成

2024年5月29日(水) 13:45 〜 15:15 展示場特設会場 (2) (幕張メッセ国際展示場 6ホール)

コンビーナ:山本 衛(京都大学生存圏研究所)、小川 泰信(国立極地研究所)、野澤 悟徳(名古屋大学宇宙地球環境研究所)、吉川 顕正(九州大学大学院理学研究院地球惑星科学部門)、座長:小川 泰信(国立極地研究所)、吉川 顕正(九州大学大学院理学研究院地球惑星科学部門)

14:30 〜 14:45

[PEM15-10] Feasibility study to estimate the ion velocity field in the F region from EISCAT_3D radar observations

*吹澤 瑞貴1小川 泰信1、西村 耕司2上野 玄太3西山 尚典1、橋本 大志1津田 卓雄4 (1.国立極地研究所、2.京都大学、3.統計数理研究所、4.電気通信大学)

キーワード:EISCAT_3D、電離圏、イオン速度、ベイズ推定

We conducted a feasibility study to estimate the horizontal ion velocity field in the ionospheric F region from ion velocities observed by the EISCAT_3D radar. We assumed a 27-beam configuration with a minimum elevation angle of 30 degrees. The ion velocity observation data from 200 km to 500 km altitude were projected to 200 km altitude, assuming that ions in this altitude range follow the E x B drift. Then, we reconstructed ion velocity vectors for ±250 km in the east-west direction and ±500 km in the north-south direction at 200 km altitude. The resolution in north-south and east-west directions was 25 km. The reconstruction was conducted by maximizing a posterior probability based on Bayes’ theorem. The constraints were set to minimize the L2 norms of the following four vectors in the horizontal plane: (1) the first and (2) the second derivative of three components of the ion velocity vector, (3) the divergence of the ion velocity perpendicular to the magnetic field lines, and (4) the ion velocity parallel to the magnetic field lines. We investigated which combination of the four constraints would reconstruct the shear flow field most correctly and found that the best combination was (2), (3), and (4). Weighting factors for each term were determined by the 5-fold cross-validation method.