Japan Geoscience Union Meeting 2019

Presentation information

[E] Poster

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

[P-EM13] Inner magnetosphere: Recent understanding and new insights

Wed. May 29, 2019 3:30 PM - 5:00 PM Poster Hall (International Exhibition Hall8, Makuhari Messe)

convener:Yusuke Ebihara(Research Institute for Sustainable Humanosphere, Kyoto University), Danny Summers(Memorial University of Newfoundland), Yoshizumi Miyoshi(Institute for Space-Earth Environmental Research, Nagoya University), Shinji Saito(Graduate School of Science, Nagoya University)

[PEM13-P09] Relativistic electron acceleration by whistler-mode chorus waves in 1D, 2D, and 3D magnetic field models.

*Keita Takahashi1, Yoshiharu Omura1, Yikai HSIEH1, Danny Summers2 (1.Research Institute for Sustainable Humanosphere, Kyoto University , 2.Department of Mathematics and Statistics, Memorial University of Newfoundland)

We evaluate the acceleration efficiencies of relativistic electrons under a 1D, 2D, and 3D model magnetic fields. We perform test-particle simulations and analyze nonlinear trapping motions of resonant electrons in each model. As a chorus wave model, we assume that a chorus wave packet generated at the magnetic equator propagates along the magnetic field to higher latitudes. When we perform simulations with the whistler mode wave, the cyclotron resonance with energetic electrons occurs at the similar timing in each model. Although we find relativistic turning acceleration (RTA) [1] to take place in each model, acceleration efficiencies of resonant electrons are different in these models. In terms of the numerical Green’s function[2], we find a clear difference in time evolution of the distribution function in energy and equatorial pitch angle. The energy gap between resonant electrons and non-resonant electrons in the 1D model is slightly different from those in the 2D and 3D models. The energy gap in the 3D model is the largest among the three magnetic field models. This difference is due to additional oscillations in the velocity phase space, which only occur in the 2D and 3D models. These oscillations occur because the magnitude of the magnetic field changes during one period of relativistic cyclotron motion, affecting the nonlinear trapping conditions of resonant electrons.


[1] Y. Omura, N. Furuya, D. Summers, Relativistic turning acceleration of resonant electrons by coherent whistler-mode waves in a dipole magnetic field, Journal Geophysical Research, Vol. 112, A06236, doi:10.1029/2006JA012243, 2007.

[2] Y. Omura, Y. Miyashita, M. Yoshikawa, D. Summers, M. Hikishima, Y. Ebihara, and Y. Kubota (2015), Formation process of relativistic electron flux through interaction with chorus emissions in the Earth’s inner magnetosphere, J. Geophys. Res. Space Physics, 120, 9545–9562, doi:10.1002/2015JA021563, 2015.