Japan Geoscience Union Meeting 2015

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International Session (Oral)

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

[P-EM09] Dynamics in magnetosphere and ionosphere

Wed. May 27, 2015 4:15 PM - 5:00 PM 302 (3F)

Convener:*Shin'ya Nakano(The Institute of Statistical Mathematics), Yoshizumi Miyoshi(Solar-Terrestrial Environement Laboratory, Nagoya University), Hiroshi Hasegawa(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency), Yoshimasa Tanaka(National Institute of Polar Research), Tomoaki Hori(Nagoya University Solar Terrestrial Environment Laboratory Geospace Research Center), Chair:Yuki Obana(Department of Engineering Science, Faculty of Engineering, Osaka Electro-Communication University)

4:45 PM - 4:48 PM

[PEM09-P06] Features of long period geomagnetic pulsations caused by the inclined front of the solar wind discontinuity

3-min talk in an oral session

Yulia KLIBANOVA1, Vladimir MISHIN1, B. TSEGMED2, *Aleksei MOISEEV3 (1.Institute of Solar-Terrestrial Physics Siberian Branch RAS, Irkutsk, Russia, 2.Research Center for Astronomy and Geophysics, Academy of Sciences of Mongolia, Ulan Bator, 3.Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, SB RAS, Yakutsk, Russia)

Keywords:geomagnetic pulsations, ULF waves, solar wind discontinuity, wave propagation

We study long-period geomagnetic pulsations caused by the solar wind discontinuity impact during the July 14, 2012 magnetic storm onset from data of satellite observations in the solar wind and magnetosphere, as well as of ground stations located at low, middle and high latitudes. The character of pulsations propagation is shown to correspond to their excitation mechanism by the discontinuity front at the magnetopause. Location relative to the noon of the sector, from which the waves propagate to both magnetosphere flanks, is determined by the front azimuthal angle inclination. We discuss a change of polarization both by longitude and latitude directions. The frequency of spectral maximum of the pulsations does not coincide with one of the solar wind oscillations.