Japan Geoscience Union Meeting 2015

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International Session (Poster)

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

[P-EM07] Space Weather, Space Climate, and VarSITI

Tue. May 26, 2015 6:15 PM - 7:30 PM Convention Hall (2F)

Convener:*Ryuho Kataoka(National Institute of Polar Research), Yusuke Ebihara(Research Institute for Sustainable Humanosphere, Kyoto University), Yoshizumi Miyoshi(Solar-Terrestrial Environement Laboratory, Nagoya University), Toshifumi Shimizu(Institute of Space and Astronautical Science, JAXA), Ayumi Asai(Unit for Synergetic Studies of Space, Kyoto University), Hidekatsu Jin(National Institude of Information and Communications Technology), Tatsuhiko Sato(Japan Atomic Energy Agency), Kanya Kusano(Solar-Terrestrial Environment Laboratory, Nagoya University), Hiroko Miyahara(College of Art and Design, Musashino Art University), Takuji Nakamura(National Institute of Polar Research), Kazuo Shiokawa(Solar-Terrestrial Environment Laboratory, Nagoya University), Kiminori Itoh(Graduate School of Engineering, Yokohama National University)

6:15 PM - 7:30 PM

[PEM07-P05] Characteristics of equatorial Pc 5 observed by the MAGDAS network under high-speed solar wind conditions

*Kaisei AKIMOTO1, Akiko FUJIMOTO2, Akimasa YOSHIKAWA1, Teiji UOZUMI2, Shuji ABE2 (1.Department of Earth and Planetary Sciences Graduate school of Sciences Kyushu University, 2.International Center for Space Weather Science and education)

Keywords:MAGDAS, dip equator, Pc 5

While investigating auroral latitude Pc 5 pulsations, Baker et al. (2003) and Mathie and Mann et al. (2001) found that these pulsations have a good correlation with the solar wind flow speed. Also, Mathie and Mann et al. (2000) found that auroral latitude Pc 5 is related to relativistic electron flux variation in the radiation belt. There are many studies about the characteristics of auroral latitude Pc 5, while equatorial Pc 5 received little attention because there are fewer observation points in the equatorial region. So, we investigated the characteristics of equatorial Pc 5 under high-speed solar wind conditions by using the data from dip equator stations of the MAGDAS/CPMN network (Kyushu University) during 2005/01/01 ~2013/12/31. We found that electron flux enhancement is preceded by an intense activity of Pc 5 at the dayside equatorial MAGDAS stations during 2010/08/24~2010/08/27. Reeves et al. (2003) showed that different types of relativistic electron flux variation are observed after geomagnetic disturbances such as magnetic storm (i.e. not only increase type but also no-change type and decrease type).We statistically analyzed the dependence of equatorial Pc 5 pulsations on the relativistic electron flux variation.