| Issue |
EPJ Web Conf.
Volume 235, 2020
XLIX International Symposium on Multiparticle Dynamics (ISMD 2019)
|
|
|---|---|---|
| Article Number | 07003 | |
| Number of page(s) | 6 | |
| Section | Cosmic Ray and Astroparticle Physics | |
| DOI | https://doi.org/10.1051/epjconf/202023507003 | |
| Published online | 16 June 2020 | |
https://doi.org/10.1051/epjconf/202023507003
Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
1 Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico, 87545, USA
2 Department of Physics and Astronomy, Rice University, Houston, Texas 77005, USA
★ e-mail: yclu@lanl.gov
Published online: 16 June 2020
A rotating pulsar creates a surrounding pulsar wind nebula (PWN) by steadily releasing an energetic wind into the interior of the expanding shockwave of supernova remnant or interstellar medium. At the termination shock of a PWN, the Poynting-flux- dominated relativistic striped wind is compressed. Magnetic reconnection is driven by the compression and converts magnetic energy into particle kinetic energy and accelerating particles to high energies. We carrying out particle-in-cell (PIC) simulations to study the shock structure as well as the energy conversion and particle acceleration mechanism. By analyzing particle trajectories, we find that many particles are accelerated by Fermi-type mechanism. The maximum energy for electrons and positrons can reach hundreds of TeV.
© The Authors, published by EDP Sciences, 2020
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