Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations

Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations

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....

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Main Authors: Lu Yingchao, Guo Fan, Kilian Patrick, Li Hui, Huang Chengkun, Liang Edison
Format: Article
Language:English
Published: EDP Sciences 2020-01-01
Series:EPJ Web of Conferences
Online Access:https://www.epj-conferences.org/articles/epjconf/pdf/2020/11/epjconf_ismd2019_07003.pdf
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spelling doaj-81bf7e9e20e24daf93766892c5f075c02021-08-02T13:30:46ZengEDP SciencesEPJ Web of Conferences2100-014X2020-01-012350700310.1051/epjconf/202023507003epjconf_ismd2019_07003Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulationsLu YingchaoGuo Fan0Kilian Patrick1Li Hui2Huang Chengkun3Liang Edison4 Theoretical Division, Los Alamos National Laboratory Theoretical Division, Los Alamos National Laboratory Theoretical Division, Los Alamos National Laboratory Theoretical Division, Los Alamos National Laboratory Department of Physics and Astronomy, Rice UniversityA 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.https://www.epj-conferences.org/articles/epjconf/pdf/2020/11/epjconf_ismd2019_07003.pdf
collection DOAJ
language English
format Article
sources DOAJ
author Lu Yingchao
Guo Fan
Kilian Patrick
Li Hui
Huang Chengkun
Liang Edison
spellingShingle Lu Yingchao
Guo Fan
Kilian Patrick
Li Hui
Huang Chengkun
Liang Edison
Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
EPJ Web of Conferences
author_facet Lu Yingchao
Guo Fan
Kilian Patrick
Li Hui
Huang Chengkun
Liang Edison
author_sort Lu Yingchao
title Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
title_short Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
title_full Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
title_fullStr Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
title_full_unstemmed Studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
title_sort studying particle acceleration from driven magnetic reconnection at the termination shock of a relativistic striped wind using particle-in-cell simulations
publisher EDP Sciences
series EPJ Web of Conferences
issn 2100-014X
publishDate 2020-01-01
description 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.
url https://www.epj-conferences.org/articles/epjconf/pdf/2020/11/epjconf_ismd2019_07003.pdf
work_keys_str_mv AT luyingchao studyingparticleaccelerationfromdrivenmagneticreconnectionattheterminationshockofarelativisticstripedwindusingparticleincellsimulations
AT guofan studyingparticleaccelerationfromdrivenmagneticreconnectionattheterminationshockofarelativisticstripedwindusingparticleincellsimulations
AT kilianpatrick studyingparticleaccelerationfromdrivenmagneticreconnectionattheterminationshockofarelativisticstripedwindusingparticleincellsimulations
AT lihui studyingparticleaccelerationfromdrivenmagneticreconnectionattheterminationshockofarelativisticstripedwindusingparticleincellsimulations
AT huangchengkun studyingparticleaccelerationfromdrivenmagneticreconnectionattheterminationshockofarelativisticstripedwindusingparticleincellsimulations
AT liangedison studyingparticleaccelerationfromdrivenmagneticreconnectionattheterminationshockofarelativisticstripedwindusingparticleincellsimulations
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