Japan Geoscience Union Meeting 2016

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International Session (Oral)

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

[P-EM07] Dynamics in magnetosphere and ionosphere

Wed. May 25, 2016 9:00 AM - 10:30 AM 103 (1F)

Convener:*Yoshizumi Miyoshi(Institute for Space-Earth Environmental Research, Nagoya University), Yoshimasa Tanaka(National Institute of Polar Research), Aoi Nakamizo(Applied Electromagnetic Research Institute, National Institute of Information and Communications Technology), Mitsunori Ozaki(Faculty of Electrical and Computer Engineering, Institute of Science and Engineering, Kanazawa University), Shin'ya Nakano(The Institute of Statistical Mathematics), Tomoaki Hori(Institute for Space-Earth Environmental Research, Nagoya University), Chair:Yoshimasa Tanaka(National Institute of Polar Research)

9:30 AM - 9:45 AM

[PEM07-15] Statistical feature of Omega band aurora observed by THEMIS all-sky imager network

*Natsuo Sato1,2, Akira Kadokura1,2, Yoshimasa Tanaka1,2, Tomoaki Hori3, Akira Sessai Yukimatu1,3 (1.National Institute of Polar Research, 2.SOKENDAI, 3.Institute for Space-Earth Environment Research, Nagoya University)

Keywords:aurora, omega band aurora, magnetosphere, ionosphere, magnetosphere-ionosphere coupling, polar region

We examine morphological and statistical characteristics of Omega band auroras. In order to study statistical feature of Omega band aurora we used the THEMIS ground-based all-sky imager network data for 8 years from January 2007 to December 2014. Omega band auroras show their own distinctive behavior on shape and movement, so we could easily pick up an Omega band auroral event from the THEMIS summary plot database on keogram and all-sky image. Consequently, we could identify ~330 events of Omega band type auroras.
In this study we examine statistical features for the following parameters when Omega aurora observed; 1) magnetic local time (MLT), 2) seasonal variations, 3) annual variations, 4) life time, 5) drift speed, 6) scale size, 7) Kp and AE index dependence, 8) solar wind speed and pressure, 9) IMF By and Bz dependence. Then we will discuss their signature.