TY - JOUR
T1 - Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
AU - Tomita, Sara
AU - Ohira, Yutaka
AU - Kimura, Shigeo S.
AU - Tomida, Kengo
AU - Toma, Kenji
N1 - Funding Information:
We thank A. Kuwata, R. Kuze, Y. Matsumoto, and M. Kobayashi for useful comments. The software used in this work was developed by Y. Matsumoto. Numerical computations were carried out on Cray XC50 at the Center for Computational Astrophysics, National Astronomical Observatory of Japan. This work is supported by JSPS KAKENHI grant Nos. 19H01893 (Y.O.), 19J00198 (S.S.K.), 21H04487 (K. Tomida and Y.O.), and 18H01245 (K. Toma). Y.O. is supported by the Leading Initiative for Excellent Young Researchers, MEXT, Japan. S.S.K. acknowledges support from the Tohoku Initiative for Fostering Global Researchers for Interdisciplinary Sciences (TI-FRIS), from MEXT’s Strategic Professional Development Program for Young Researchers.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/9/1
Y1 - 2022/9/1
N2 - 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.
AB - 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.
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U2 - 10.3847/2041-8213/ac88be
DO - 10.3847/2041-8213/ac88be
M3 - Article
AN - SCOPUS:85137723185
SN - 2041-8205
VL - 936
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L9
ER -