Japan Geoscience Union Meeting 2016

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International Session (Poster)

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

[P-EM04] Space Weather, Space Climate, and VarSITI

Sun. May 22, 2016 5:15 PM - 6:30 PM Poster Hall (International Exhibition Hall HALL6)

Convener:*Ryuho Kataoka(National Institute of Polar Research), Antti Pulkkinen(NASA GSFC), Yusuke Ebihara(Research Institute for Sustainable Humanosphere, Kyoto University), Yoshizumi Miyoshi(Institute for Space-Earth Environmental Research, 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(Institute for Space-Earth Environmental Research, Nagoya University), Hiroko Miyahara(College of Art and Design, Musashino Art University), Kiminori Itoh(Graduate School of Engineering, Yokohama National University), Kazuo Shiokawa(Institute for Space-Earth Environmental Research, Nagoya University), Takuji Nakamura(National Institute of Polar Research), Shigeo Yoden(Division of Earth and Planetary Sciences, Graduate School of Science, Kyoto University), Kiyoshi Ichimoto(Kwasan and Hida Observatories, Kyoto University), Mamoru Ishii(National Institute of Information and Communications Technology)

5:15 PM - 6:30 PM

[PEM04-P12] Relationship between solar wind dynamic pressure and amplitude of geomagnetic sudden commencement (SC)

*Tohru Araki1, Atsuki Shinbori2 (1.Formerly Kyoto Univ., 2.RISH, Kyoto Univ.)

Keywords:geomagnetic sudden commencement(SC), solar wind dynamic pressure , , ionospheric current, field aligned current, LT variation, Siscoe’s relationship

Although the primary cause of the geomagnetic sudden commencement (SC) is the enhanced magnetopause current, induced field aligned currents, ionospheric currents and earth currents produce a complex global distribution of the amplitude and waveform of SC. As the result the SC amplitude shows a clear latitudinal and local time variation. These variations have not been taken into account in the Siscoe’s linear relationship ( dH = C* d( Pd**0.5 )) which connects the SC amplitude (dH) with the corresponding dynamic pressure (Pd) variation of the solar wind.
By considering the physical background of SC we studied which local time is best to extract the information of the solar wind dynamic pressure and concluded that the SC amplitude at 4-5h local time of middle- and low-latitude stations most directly reflects the dynamic pressure effect.
This result is used to re-check the order of magnitude of the largest 3 SCs ( dH > 200 nT at Kakioka) observed since 1868 (Araki, 2015). The SC occurred on March 24, 1940 still keeps the first rank even if
the LT variation is taken into account.