Japan Geoscience Union Meeting 2018

Presentation information

[EE] Oral

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

[P-EM16] Dynamics of Earth's Inner Magnetosphere and Initial Results from Arase

Mon. May 21, 2018 3:30 PM - 5:00 PM 303 (3F International Conference Hall, Makuhari Messe)

convener:Danny Summers(Memorial University of Newfoundland), Yoshizumi Miyoshi(Institute for Space-Earth Environmental Research, Nagoya University), Keisuke Hosokawa(電気通信大学大学院情報理工学研究科, 共同), Yusuke Ebihara(Research Institute for Sustainable Humanosphere, Kyoto University), Chairperson:Ebihara Yusuke(RISH, Kyoto University)

4:00 PM - 4:15 PM

[PEM16-15] Pc4 ULF waves and proton flux oscillations observed by the Arase satellite in the morning sector during satellite-ground conjunction: Evidence for giant pulsations

*Kazuhiro Yamamoto1, Masahito Nose1, Satoshi Kasahara2, Shoichiro Yokota3, Kunihiro Keika2, Ayako Matsuoka4, Mariko Teramoto5, Reiko Nomura4, Kazue Takahashi6, Massimo Vellante7, Balazs Heilig8, Akiko Fujimoto9, Yoshimasa Tanaka10, Manabu Shinohara11, Iku Shinohara4, Yoshizumi Miyoshi5 (1.Graduate School of Science, Kyoto University, 2.The University of Tokyo, 3.Osaka University, 4.Japan Aerospace Exploration Agency, 5.Nagoya University, 6.Johns Hopkins University Applied Physics Laboratory, 7.University of L'Aquila, 8.Geological and Geophysical Institute of Hungary, 9.Kyushu University, 10.National Institute of Polar Research, 11.National Institute of Technology, Kagoshima College)

Keywords:ULF waves, giant pulsations, drift resonance, Arase satellite, ring current

We studied interaction between westward propagating ULF waves and energetic protons observed in the morning sector by the Arase satellite and ground magnetometers on April 15, 2017. Arase was passing the equatorial region during 01-02 UT and found that the compressional component of the magnetic field was oscillating at a frequency of 12.5 mHz. Proton flux at energy of > ~70 keV and pitch angles around 90° was also oscillating at the same frequency. By using a finite Larmor effect that appeared in proton flux observation, we estimated the azimuthal wave number (m number) to be -30 to -40. We also studied wave polarization and m number using data from the European quasi-Meridional Magnetometer Array (EMMA) [Lichtenberger et al., 2013]. A polarization reversal from counter clockwise at low latitude to clockwise at high latitudes was detected at Ranua (MLAT = 62.1°), Ivalo (MLAT = 65.1°), and Kevo (MLAT = 66.3°). This is one of the common properties of giant pulsations (Pgs) observed on the ground. The estimated m number is -30 to -50, slightly higher than those reported in previous studies [e.g., Takahashi et al., 1992; Chisham et al.,1997; Glassmeier et al., 1990; Motoba et al., 2015]. The eigen-frequency of the field line at the Arase satellite obtained using the MHD wave equation derived by Singer et al. [1981] suggests that the waves were excited at the fundamental mode. The pitch angle dependence of proton flux oscillations also implies odd mode waves according to Southwood and Kivelson [1981]. We theoretically estimated the m number to be -47 from a drift resonance signature, an amplitude peak of proton flux oscillations at 109.6 keV. Since this m value is comparable to those obtained using the other methods, the drift resonance between fundamental mode ULF waves and ~100 keV protons is considered to be present in this event. In addition, we found intensification of the radial gradient of proton phase space density at 109.6 keV, which can explain the excitation of the observed waves. The time evolution of the unstable distribution suggests a causal relationship between the ULF waves and energetic protons.