Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
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DOI：
10.3847/2041-8213/ac88be
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发表时间：
2022-04
期刊：
影响因子：
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通讯作者：
S. Tomita;Y. Ohira;S. Kimura;K. Tomida;K. Toma
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文献类型：
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作者：
S. Tomita;Y. Ohira;S. Kimura;K. Tomida;K. Toma
相对论性磁化无碰撞激波和致密团块之间的相互作用被认为在磁场放大和宇宙射线加速中起着至关重要的作用。我们首次使用二维粒子池（PIC）模拟来研究这一过程，其中团块大小远远大于下游粒子的陀螺半径。我们还进行了相同条件下的相对论磁流体动力学（MHD）模拟，以观察动力学效应。在PIC模拟中，粒子沿磁力线从激波团块中逸出，使得涡度低于MHD模拟。此外，在PIC和MHD模拟中，由于相对论效应，激波团块快速减速。在相对论性无碰撞激波中，由于逃逸和减速，激波团块不能放大下游磁场。这种大规模的PIC模拟为理解无碰撞等离子体系统的大规模行为打开了一扇新的窗口。
The interactions between a relativistic magnetized collisionless shock and dense clumps have been expected to play a crucial role in magnetic field amplification and cosmic-ray acceleration. We investigate this process using two-dimensional Particle-In-Cell (PIC) simulations, for the first time, where the clump size is much larger than the gyroradius of the downstream particles. We also perform relativistic magnetohydrodynamic (MHD) simulations for the same condition, to see the kinetic effects. We find that particles escape from the shocked clump along magnetic field lines in the PIC simulations, so that the vorticity is lower than that in the MHD simulations. Moreover, in both the PIC and MHD simulations, the shocked clump quickly decelerates because of relativistic effects. Owing to the escape and the deceleration, the shocked clump cannot amplify the downstream magnetic field in relativistic collisionless shocks. This large-scale PIC simulation opens a new window to understanding large-scale behaviors in collisionless plasma systems.