[P-EM17] 宇宙プラズマ理論・シミュレーション

[PEM17-13] ホイッスラー乱流中での運動論スケール静電波動の励起について: 粒子シミュレーション

*齊藤 慎司¹、成行 泰裕³、梅田 隆行² (1.名古屋大学　大学院理学研究科、2.名古屋大学　宇宙地球環境研究所、3.富山大学　人間発達科学部)

キーワード：プラズマ乱流、ホイッスラー波、粒子シミュレーション

Solar wind observations show that larger cascade rates of turbulence lead to steeper power-law magnetic spectra at kinetic scales. This suggests that larger fluctuation amplitudes at kinetic scales lead to some nonlinear properties more efficiently. Our previous research showed that the modified two stream instability in a monochromatic finite amplitude whistler wave contributes the nonlinear dissipation of the wave at kinetic scales. This result suggests that kinetic instabilities can enhance the dissipation at electron and ion scales. The wave driven instability occurs with larger wave amplitudes more efficiently, so this process could be a contributor for the steep power-law spectrum at kinetic scales. Here two-dimensional electromagnetic particle-in-cell simulations in magnetized, homogeneous, collisionless electron-ion plasma demonstrate the forward cascade of whistler turbulence at ion scales. The simulation show that whistler turbulence cascades into electron scales, and show a spectrum break around the scale of the electron inertial length. Around the scale related to the break point, electrostatic fluctuations appear at several points intermittently. The electrostatic fluctuations are expected to be driven by ion acoustic instability driven by localized electric current in whistler turbulence. We will discuss the instability driven dissipation of whistler turbulence at kinetic scales and heating of both electrons and ions.