日本地球惑星科学連合2019年大会

講演情報

[E] ポスター発表

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-EM10] Multi-scale Coupling in the Magnetosphere-Ionosphere-Thermosphere System

2019年5月27日(月) 17:15 〜 18:30 ポスター会場 (幕張メッセ国際展示場 8ホール)

コンビーナ:Yue Deng(University of Texas at Arlington)、Toshi Nishimura(Boston University)、Liu Huixin(九州大学理学研究院地球惑星科学専攻 九州大学宙空環境研究センター)、Yanshi Huang(Harbin Institute of Technology, Shenzhen)

[PEM10-P02] Comparison of precipitating particle energy of proton aurora at geomagnetic conjugate points

*田口 真1西島 樹1門倉 昭2 (1.立教大学、2.情報・システム研究機構)

It is expected that mirror images of aurora are observed at geomagnetic conjugate points in the northern and southern auroral zones connected by a geomagnetic field line. However, geomagnetic conjugate auroras often show non-conjugacy, which reflects north-south asymmetry of the solar wind, the magnetosphere and the ionospheres. In other words acceleration mechanism of auroral particles may be studied by comparing aurora simultaneously occurring at geomagnetic conjugate points. A hydrogen Balmer beta emission at the wavelength of 486.1 nm which is the brightest among the proton auroral lines was observed at a pair of geomagnetic conjugate points to compare precipitating particle energy. Two identical Proton Auroral Specrographs (PASs) which obtain auroral spectra along a geomagnetic meridian at a rate of 1 image/min were installed at Tjornes in Iceland and Syowa Station in Antarctica. Data obtained during a period from September 4, 2018 to October 9, 2018 were analyzed to derive an average kinetic energy of precipitating protons along a local geomagnetic field line from a Doppler shift of the H beta line. As a result we are succeeded in simultaneous observations of proton auroras at both conjugate points in 5 nights on September 4, 5, 6, 7 , and 10. The average energies of precipitating protons range from 0 keV to 7 keV, and sometimes show a periodical variation with a period of 4 - 5 min. Conjugacy of precipitating particle energy will be discussed in the presentation.