Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump

被引：4

作者：

Tomita, Sara ^{[1
,2
]}

Ohira, Yutaka ^{[3
]}

Kimura, Shigeo S. ^{[1
,2
]}

Tomida, Kengo ^{[2
]}

Toma, Kenji ^{[1
,2
]}

机构：

[1] Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Sendai, Miyagi 9808578, Japan

[2] Tohoku Univ, Grad Sch Sci, Astron Inst, Sendai, Miyagi 9808578, Japan

[3] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2022年 / 936卷 / 01期

关键词：

FIELD AMPLIFICATION; PARTICLE-ACCELERATION; SUPERNOVA REMNANT; TURBULENCE; ENERGY; WAVE; INSTABILITIES; EMISSION; PLASMA;

D O I：

10.3847/2041-8213/ac88be

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：6

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