Japan Geoscience Union Meeting 2018

Presentation information

[EE] Oral

P (Space and Planetary Sciences) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM15] Dynamics in magnetosphere and ionosphere

Sun. May 20, 2018 9:00 AM - 10:30 AM 303 (3F International Conference Hall, Makuhari Messe)

convener:Yoshimasa Tanaka(National Institute of Polar Research), Tomoaki Hori(Institute for Space-Earth Environmental Research, Nagoya University), Aoi Nakamizo(情報通信研究機構 電磁波研究所, 共同), Mitsunori Ozaki(Faculty of Electrical and Computer Engineering, Institute of Science and Engineering, Kanazawa University), Chairperson:Shinbori Atsuki(ISEE, Nagoya Univ.), Sato Yuka(National Institute of Polar Research)

9:15 AM - 9:30 AM

[PEM15-02] Red line aurora in the dayside cusp for northward IMF

*Satoshi Taguchi1, Yushin Oda1, Keisuke Hosokawa2 (1.Department of Geophysics, Graduate School of Science, Kyoto University, 2.Department of Communication Engineering and Informatics, University of Electro-Communications)

Keywords:cusp, aurora, electron precipitation, solar wind

During northward IMF magnetosheath electrons and ions are injected into the cusp along open magnetic field lines after reconnection poleward of the cusp. It is well understood that the injected ions often produce the dayside proton auroral spot at ionospheric heights, and that its brightness increases as the solar wind dynamic pressure becomes high. It remains unclear to what extent the injected electrons, which produce red line cusp auroras, reflect solar wind parameters including the dynamic pressure. In this study we examined relationships of red line cusp aurora emissions during northward IMF to solar wind parameters by using observations of cusp auroras from an all-sky imager at Longyearbyen, Svalbard, and observations of precipitating particles from the DMSP spacecraft traversing the region above the cusp auroras. Results of analyses show that the average component of the red line aurora emissions tends to increase with the solar wind speed, not the solar wind density or the dynamic pressure. We interpret this relationship in terms of the electron velocity distribution in the solar wind.