Particle-in-cell simulations of magnetic reconnection in laser-plasma experiments on Shenguang-II facility

2013 ◽  
Vol 20 (11) ◽  
pp. 112110 ◽  
Author(s):  
San Lu ◽  
Quanming Lu ◽  
Quanli Dong ◽  
Can Huang ◽  
Shui Wang ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Laser Plasma ◽  
Particle In Cell

scholarly journals PIC methods in astrophysics: simulations of relativistic jets and kinetic physics in astrophysical systems

2021 ◽  
Vol 7 (1) ◽  
Author(s):  
Kenichi Nishikawa ◽  
Ioana Duţan ◽  
Christoph Köhn ◽  
Yosuke Mizuno
Keyword(s):  
Plasma Physics ◽  
Magnetic Reconnection ◽  
Laser Plasma ◽  
High Performance ◽  
Relativistic Jets ◽  
Astrophysical Plasmas ◽  
Computing Power ◽  
Particle In Cell ◽  
The Future ◽  
Pic Method

AbstractThe Particle-In-Cell (PIC) method has been developed by Oscar Buneman, Charles Birdsall, Roger W. Hockney, and John Dawson in the 1950s and, with the advances of computing power, has been further developed for several fields such as astrophysical, magnetospheric as well as solar plasmas and recently also for atmospheric and laser-plasma physics. Currently more than 15 semi-public PIC codes are available which we discuss in this review. Its applications have grown extensively with increasing computing power available on high performance computing facilities around the world. These systems allow the study of various topics of astrophysical plasmas, such as magnetic reconnection, pulsars and black hole magnetosphere, non-relativistic and relativistic shocks, relativistic jets, and laser-plasma physics. We review a plethora of astrophysical phenomena such as relativistic jets, instabilities, magnetic reconnection, pulsars, as well as PIC simulations of laser-plasma physics (until 2021) emphasizing the physics involved in the simulations. Finally, we give an outlook of the future simulations of jets associated to neutron stars, black holes and their merging and discuss the future of PIC simulations in the light of petascale and exascale computing.

Particle-in-Cell Simulations of Fast Magnetic Reconnection in Laser-Plasma Interaction

2013 ◽  
Vol 30 (4) ◽  
pp. 045201 ◽  
Author(s):  
Ze-Chen Zhang ◽  
Quan-Ming Lu ◽  
Quan-Li Dong ◽  
San Lu ◽  
Can Huang ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Laser Plasma ◽  
Plasma Interaction ◽  
Laser Plasma Interaction ◽  
Particle In Cell

scholarly journals Brief Communication: The double layer in the separatrix region during magnetic reconnection

2015 ◽  
Vol 22 (2) ◽  
pp. 167-171
Author(s):  
J. Guo ◽  
B. Yu
Keyword(s):  
Electron Beam ◽  
Magnetic Reconnection ◽  
Double Layer ◽  
Particle In Cell ◽  
Acoustic Instability ◽  
Ion Acoustic ◽  
Evolution Stage ◽  
Spatial Size ◽  
Electron Holes ◽  
Observation Results

Abstract. With two-dimensional (2-D) particle-in-cell (PIC) simulations we investigate the evolution of the double layer (DL) driven by magnetic reconnection. Our results show that an electron beam can be generated in the separatrix region as magnetic reconnection proceeds. This electron beam could trigger the ion-acoustic instability; as a result, a DL accompanied with electron holes (EHs) can be found during the nonlinear evolution stage of this instability. The spatial size of the DL is about 10 Debye lengths. This DL propagates along the magnetic field at a velocity of about the ion-acoustic speed, which is consistent with the observation results.

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

2020 ◽  
Vol 235 ◽  
pp. 07003
Author(s):  
Yingchao Lu ◽  
Fan Guo ◽  
Patrick Kilian ◽  
Hui Li ◽  
Chengkun Huang ◽  
...  
Keyword(s):  
Particle Acceleration ◽  
Magnetic Reconnection ◽  
Magnetic Energy ◽  
Maximum Energy ◽  
Termination Shock ◽  
Particle In Cell ◽  
Poynting Flux ◽  
Electrons And Positrons ◽  
Particle Kinetic Energy ◽  
Fermi Type

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.

High-order Particle-In-Cell simulations of laser-plasma interaction

2019 ◽  
Vol 227 (14) ◽  
pp. 1603-1614 ◽  
Author(s):  
Stephen M. Copplestone ◽  
Marcel Pfeiffer ◽  
Stefanos Fasoulas ◽  
Claus-Dieter Munz
Keyword(s):  
Laser Plasma ◽  
High Order ◽  
Plasma Interaction ◽  
Laser Plasma Interaction ◽  
Particle In Cell

Particle-in-Cell modelling of laser–plasma interaction using Fourier decomposition

2009 ◽  
Vol 228 (5) ◽  
pp. 1803-1814 ◽  
Author(s):  
A.F. Lifschitz ◽  
X. Davoine ◽  
E. Lefebvre ◽  
J. Faure ◽  
C. Rechatin ◽  
...  
Keyword(s):  
Laser Plasma ◽  
Plasma Interaction ◽  
Fourier Decomposition ◽  
Laser Plasma Interaction ◽  
Particle In Cell

Reconnection Front Associated with Asymmetric Magnetic Reconnection: Particle-in-cell Simulations

2019 ◽  
Vol 881 (1) ◽  
pp. L22 ◽  
Author(s):  
Liangjin Song ◽  
Meng Zhou ◽  
Yongyuan Yi ◽  
Xiaohua Deng ◽  
Zhihong Zhong
Keyword(s):  
Magnetic Reconnection ◽  
Particle In Cell

scholarly journals Kinetic beaming in radiative relativistic magnetic reconnection: a mechanism for rapid gamma-ray flares in jets

2020 ◽  
Vol 498 (1) ◽  
pp. 799-820 ◽  
Author(s):  
J M Mehlhaff ◽  
G R Werner ◽  
D A Uzdensky ◽  
M C Begelman
Keyword(s):  
Magnetic Reconnection ◽  
Gamma Ray ◽  
Critical Role ◽  
High Energy ◽  
Particle In Cell ◽  
Pair Plasma ◽  
Spectrum Radio ◽  
Inverse Compton ◽  
Emission Models ◽  
The One

ABSTRACT Rapid gamma-ray flares pose an astrophysical puzzle, requiring mechanisms both to accelerate energetic particles and to produce fast observed variability. These dual requirements may be satisfied by collisionless relativistic magnetic reconnection. On the one hand, relativistic reconnection can energize gamma-ray emitting electrons. On the other hand, as previous kinetic simulations have shown, the reconnection acceleration mechanism preferentially focuses high energy particles – and their emitted photons – into beams, which may create rapid blips in flux as they cross a telescope’s line of sight. Using a series of 2D pair-plasma particle-in-cell simulations, we explicitly demonstrate the critical role played by radiative (specifically inverse Compton) cooling in mediating the observable signatures of this ‘kinetic beaming’ effect. Only in our efficiently cooled simulations do we measure kinetic beaming beyond one light crossing time of the reconnection layer. We find a correlation between the cooling strength and the photon energy range across which persistent kinetic beaming occurs: stronger cooling coincides with a wider range of beamed photon energies. We also apply our results to rapid gamma-ray flares in flat-spectrum radio quasars, suggesting that a paradigm of radiatively efficient kinetic beaming constrains relevant emission models. In particular, beaming-produced variability may be more easily realized in two-zone (e.g. spine-sheath) set-ups, with Compton seed photons originating in the jet itself, rather than in one-zone external Compton scenarios.

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