scholarly journals Study of magnetic reconnection in large-scale magnetic island coalescence via spatially coupled MHD and PIC simulations

2018 ◽  
Vol 25 (8) ◽  
pp. 082904 ◽  
Author(s):  
Kirit D. Makwana ◽  
Rony Keppens ◽  
Giovanni Lapenta
Keyword(s):  
Magnetic Reconnection ◽  
Large Scale ◽  
Magnetic Island ◽  
Island Coalescence

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

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 Large-scale Compression Acceleration during Magnetic Reconnection in a Low-β Plasma

2018 ◽  
Vol 866 (1) ◽  
pp. 4 ◽  
Author(s):  
Xiaocan Li ◽  
Fan Guo ◽  
Hui Li ◽  
Shengtai Li
Keyword(s):  
Magnetic Reconnection ◽  
Large Scale

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 Numerical study of the reconnection process between magnetic cloud and heliospheric current sheet

2018 ◽  
Vol 619 ◽  
pp. A82
Author(s):  
Man Zhang ◽  
Yu Fen Zhou ◽  
Xue Shang Feng ◽  
Bo Li ◽  
Ming Xiong
Keyword(s):  
Magnetic Reconnection ◽  
Current Sheet ◽  
Dynamic Process ◽  
Large Scale ◽  
Magnetic Cloud ◽  
Numerical Study ◽  
Three Dimensional ◽  
Heliospheric Current Sheet ◽  
Reconnection Process ◽  
Magnetic Filed

In this paper, we have used a three-dimensional numerical magnetohydrodynamics model to study the reconnection process between magnetic cloud and heliospheric current sheet. Within a steady-state heliospheric model that gives a reasonable large-scale structure of the solar wind near solar minimum, we injected a spherical plasmoid to mimic a magnetic cloud. When the magnetic cloud moves to the heliospheric current sheet, the dynamic process causes the current sheet to become gradually thinner and the magnetic reconnection begin. The numerical simulation can reproduce the basic characteristics of the magnetic reconnection, such as the correlated/anticorrelated signatures in V and B passing a reconnection exhaust. Depending on the initial magnetic helicity of the cloud, magnetic reconnection occurs at points along the boundary of the two systems where antiparallel field lines are forced together. We find the magnetic filed and velocity in the MC have a effect on the reconnection rate, and the magnitude of velocity can also effect the beginning time of reconnection. These results are helpful in understanding and identifying the dynamic process occurring between the magnetic cloud and the heliospheric current sheet.

scholarly journals Why are CMEs large-scale coronal events: nature or nurture?

2008 ◽  
Vol 26 (10) ◽  
pp. 3077-3088 ◽  
Author(s):  
L. van Driel-Gesztelyi ◽  
G. D. R. Attrill ◽  
P. Démoulin ◽  
C. H. Mandrini ◽  
L. K. Harra
Keyword(s):  
Magnetic Reconnection ◽  
Large Scale ◽  
Observational Evidence ◽  
Angular Width ◽  
Small Scale ◽  
Apparent Contradiction ◽  
Lower Corona ◽  
Magnetic Structures ◽  
Source Regions ◽  
Scale Response

Abstract. The apparent contradiction between small-scale source regions of, and large-scale coronal response to, coronal mass ejections (CMEs) has been a long-standing puzzle. For some, CMEs are considered to be inherently large-scale events – eruptions in which a number of flux systems participate in an unspecified manner, while others consider magnetic reconnection in special global topologies to be responsible for the large-scale response of the lower corona to CME events. Some of these ideas may indeed be correct in specific cases. However, what is the key element which makes CMEs large-scale? Observations show that the extent of the coronal disturbance matches the angular width of the CME – an important clue, which does not feature strongly in any of the above suggestions. We review observational evidence for the large-scale nature of CME source regions and find them lacking. Then we compare different ideas regarding how CMEs evolve to become large-scale. The large-scale magnetic topology plays an important role in this process. There is amounting evidence, however, that the key process is magnetic reconnection between the CME and other magnetic structures. We outline a CME evolution model, which is able to account for all the key observational signatures of large-scale CMEs and presents a clear picture how large portions of the Sun become constituents of the CME. In this model reconnection is driven by the expansion of the CME core resulting from an over-pressure relative to the pressure in the CME's surroundings. This implies that the extent of the lower coronal signatures match the final angular width of the CME.

scholarly journals Solar wind interaction with the Earth's magnetosphere: the role of reconnection in the presence of a large scale sheared flow

2009 ◽  
Vol 16 (1) ◽  
pp. 1-10 ◽  
Author(s):  
F. Califano ◽  
M. Faganello ◽  
F. Pegoraro ◽  
F. Valentini
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Reconnection ◽  
Large Scale ◽  
Initial Conditions ◽  
Magnetic Layer ◽  
Magnetic Islands ◽  
Solar Wind Interaction ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

Abstract. The Earth's magnetosphere and solar wind environment is a laboratory of excellence for the study of the physics of collisionless magnetic reconnection. At low latitude magnetopause, magnetic reconnection develops as a secondary instability due to the stretching of magnetic field lines advected by large scale Kelvin-Helmholtz vortices. In particular, reconnection takes place in the sheared magnetic layer that forms between adjacent vortices during vortex pairing. The process generates magnetic islands with typical size of the order of the ion inertial length, much smaller than the MHD scale of the vortices and much larger than the electron inertial length. The process of reconnection and island formation sets up spontaneously, without any need for special boundary conditions or initial conditions, and independently of the initial in-plane magnetic field topology, whether homogeneous or sheared.

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