[P-EM17] 宇宙プラズマ理論・シミュレーション

[PEM17-P06] レイリー・テイラー不安定性のブラソフシミュレーション

*和田 泰尚¹、梅田 隆行¹、町田 忍¹ (1.名古屋大学宇宙地球環境研究所)

キーワード：宇宙プラズマ、レイリー・テイラー不安定性、ブラソフシミュレーション

The Rayleigh-Taylor instability (RTI) develops at an interface between two fluids with different densities when an external force is applied from a heavy fluid to a light fluid. The RTI is seen as a secondary instability of the Kelvin-Helmholtz instability taking place at the magnetopause. The spatial scale of the secondary RTI is on the ion inertial scale or ion gyro scale where non-MHD effects are important. In the previous studies of ideal MHD simulations, the RTI develops symmetrically in the horizontal axis. On the other hand, previous hall-MHD and Finite-Larmor-Radius (FLR)-MHD simulations have shown that the RTI develops asymmetrically in the horizontal axis. In this study, basic processes of non-MHD scale RTI are of interest. We perform four-dimensional Vlasov simulations of the RTI with two spatial dimensions and two velocity dimensions. We vary the ratio of the ion inertial length and/or the ion gyro radius to the spatial scale of the density gradient layer, and discuss the effect of the non-MHD effects on the linear growth and nonlinear development of the RTI.