Plasma physics of magnetic island coalescence during magnetic reconnection

2014 ◽  
Vol 119 (8) ◽  
pp. 6177-6189 ◽  
Author(s):  
Meng Zhou ◽  
Ye Pang ◽  
Xiaohua Deng ◽  
Shiyong Huang ◽  
Xiangsheng Lai
Keyword(s):  
Plasma Physics ◽  
Magnetic Reconnection ◽  
Magnetic Island ◽  
Island Coalescence

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.

Electron acceleration via magnetic island coalescence

2009 ◽  
Author(s):  
I. Shinohara ◽  
T. Yumura ◽  
K. G. Tanaka ◽  
M. Fujimoto ◽  
Masfumi Hirahara ◽  
...  
Keyword(s):  
Electron Acceleration ◽  
Magnetic Island ◽  
Island Coalescence

scholarly journals The role of guide field in magnetic reconnection driven by island coalescence

2017 ◽  
Vol 24 (2) ◽  
pp. 022124 ◽  
Author(s):  
A. Stanier ◽  
W. Daughton ◽  
Andrei N. Simakov ◽  
L. Chacón ◽  
A. Le ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Guide Field ◽  
Island Coalescence

scholarly journals Modeling of magnetic island formation in magnetic reconnection experiment

1999 ◽  
Vol 6 (4) ◽  
pp. 1253-1257 ◽  
Author(s):  
T.-H. Watanabe ◽  
T. Hayashi ◽  
T. Sato ◽  
M. Yamada ◽  
H. Ji
Keyword(s):  
Magnetic Reconnection ◽  
Magnetic Island ◽  
Island Formation

scholarly journals ViDA: a Vlasov–DArwin solver for plasma physics at electron scales

2019 ◽  
Vol 85 (5) ◽  
Author(s):  
Oreste Pezzi ◽  
Giulia Cozzani ◽  
Francesco Califano ◽  
Francesco Valentini ◽  
Massimiliano Guarrasi ◽  
...  
Keyword(s):  
Plasma Physics ◽  
Magnetic Reconnection ◽  
Spatial Scales ◽  
Collisionless Plasma ◽  
Low Noise ◽  
Numerical Code ◽  
Small Scale ◽  
Diffusion Region ◽  
Plasma Dynamics ◽  
Algorithm Efficiency

We present a Vlasov–DArwin numerical code (ViDA) specifically designed to address plasma physics problems, where small-scale high accuracy is requested even during the nonlinear regime to guarantee a clean description of the plasma dynamics at fine spatial scales. The algorithm provides a low-noise description of proton and electron kinetic dynamics, by splitting in time the multi-advection Vlasov equation in phase space. Maxwell equations for the electric and magnetic fields are reorganized according to the Darwin approximation to remove light waves. Several numerical tests show that ViDA successfully reproduces the propagation of linear and nonlinear waves and captures the physics of magnetic reconnection. We also discuss preliminary tests of the parallelization algorithm efficiency, performed at CINECA on the Marconi-KNL cluster. ViDA will allow the running of Eulerian simulations of a non-relativistic fully kinetic collisionless plasma and it is expected to provide relevant insights into important problems of plasma astrophysics such as, for instance, the development of the turbulent cascade at electron scales and the structure and dynamics of electron-scale magnetic reconnection, such as the electron diffusion region.

PLASMA PHYSICS: Connecting Again with Magnetic Reconnection

Science ◽  
1998 ◽  
Vol 279 (5356) ◽  
pp. 1488-1489 ◽  
Author(s):  
W. M. Tang
Keyword(s):  
Plasma Physics ◽  
Magnetic Reconnection

scholarly journals On the electron dynamics during island coalescence in asymmetric magnetic reconnection

2015 ◽  
Vol 22 (9) ◽  
pp. 092901 ◽  
Author(s):  
E. Cazzola ◽  
M. E. Innocenti ◽  
S. Markidis ◽  
M. V. Goldman ◽  
D. L. Newman ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Electron Dynamics ◽  
Island Coalescence

Effect of plasma-β on the onset of plasmoid instability in Sweet–Parker current sheets

2014 ◽  
Vol 80 (5) ◽  
pp. 655-665 ◽  
Author(s):  
H. Baty
Keyword(s):  
Magnetic Reconnection ◽  
Temperature Increase ◽  
Numerical Study ◽  
Two Dimensional ◽  
Magnetic Island ◽  
Current Sheets ◽  
A Value ◽  
Similar Dependence ◽  
Definition Of ◽  
Local Temperature Increase

AbstractA numerical study of magnetic reconnection in two-dimensional resistive magnetohydrodynamics for Sweet–Parker current sheets that are subject to plasmoid instability is carried out. The effect of the initial upstream plasma-β on the critical Lundquist number Sc for the onset of plasmoid instability is studied. Our results indicate a weak dependence, with a value of Sc ≃ 1.5 × 104 in the limit of zero β, and a value of Sc ≃ 1 × 104 in the opposite high β regime (β ≫ 1). A similar dependence was previously obtained (Ni et al. 2012 Phys. Plasm. 19, 072902), but with a somewhat much larger variation, that can be largely attributed to the different configuration setup used in their study, and also to the definition of the Lundquist number. This conclusion does not depend significantly on the equilibrium used, i.e. both initial configurations with either plasma density or temperature spatial variations lead to very similar results. Finally, we show that the inner plasmoid structure appears as an under-dense hotted magnetic island, with a local temperature increase that is noticeably strengthened for low β cases.

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