Onset of collisionless magnetic reconnection in thin current sheets: Three-dimensional particle simulations

2003 ◽  
Vol 10 (9) ◽  
pp. 3521-3527 ◽  
Author(s):  
M. Scholer ◽  
I. Sidorenko ◽  
C. H. Jaroschek ◽  
R. A. Treumann ◽  
A. Zeiler
Keyword(s):  
Magnetic Reconnection ◽  
Three Dimensional ◽  
Current Sheets ◽  
Particle Simulations

Three-dimensional spontaneous magnetic reconnection in neutral current sheets

2000 ◽  
Vol 7 (1) ◽  
pp. 108-121 ◽  
Author(s):  
Jörg Schumacher ◽  
Bernhard Kliem ◽  
Norbert Seehafer
Keyword(s):  
Magnetic Reconnection ◽  
Neutral Current ◽  
Three Dimensional ◽  
Current Sheets

Toward laboratory torsional spine magnetic reconnection

2017 ◽  
Vol 83 (6) ◽  
Author(s):  
David L. Chesny ◽  
N. Brice Orange ◽  
Hakeem M. Oluseyi ◽  
David R. Valletta
Keyword(s):  
Magnetic Reconnection ◽  
Kinetic Parameters ◽  
Three Dimensional ◽  
Limited Range ◽  
Null Point ◽  
Plasma Parameters ◽  
Astrophysical Plasmas ◽  
Current Sheets ◽  
Practical Applications ◽  
Field Lines

Magnetic reconnection is a fundamental energy conversion mechanism in nature. Major attempts to study this process in controlled settings on Earth have largely been limited to reproducing approximately two-dimensional (2-D) reconnection dynamics. Other experiments describing reconnection near three-dimensional null points are non-driven, and do not induce any of the 3-D modes of spine fan, torsional fan or torsional spine reconnection. In order to study these important 3-D modes observed in astrophysical plasmas (e.g. the solar atmosphere), laboratory set-ups must be designed to induce driven reconnection about an isolated magnetic null point. As such, we consider the limited range of fundamental resistive magnetohydrodynamic (MHD) and kinetic parameters of dynamic laboratory plasmas that are necessary to induce the torsional spine reconnection (TSR) mode characterized by a driven rotational slippage of field lines – a feature that has yet to be achieved in operational laboratory magnetic reconnection experiments. Leveraging existing reconnection models, we show that within a${\lesssim}1~\text{m}^{3}$apparatus, TSR can be achieved in dense plasma regimes (${\sim}10^{24}~\text{m}^{-3}$) in magnetic fields of${\sim}10^{-1}~\text{T}$. We find that MHD and kinetic parameters predict reconnection in thin${\lesssim}20~\unicode[STIX]{x03BC}\text{m}$current sheets on time scales of${\lesssim}10~\text{ns}$. While these plasma regimes may not explicitly replicate the plasma parameters of observed astrophysical phenomena, studying the dynamics of the TSR mode within achievable set-ups signifies an important step in understanding the fundamentals of driven 3-D magnetic reconnection and the self-organization of current sheets. Explicit control of this reconnection mode may have implications for understanding particle acceleration in astrophysical environments, and may even have practical applications to fields such as spacecraft propulsion.

Turbulence-driven magnetic reconnection in the magnetosheath downstream of a quasi-parallel shock：a three-dimensional global hybrid simulation

2020 ◽  
Author(s):  
Quanming Lu ◽  
Huanyu Wang ◽  
Xueyi Wang
Keyword(s):  
Magnetic Reconnection ◽  
Electromagnetic Waves ◽  
High Speed ◽  
Three Dimensional ◽  
Hybrid Simulation ◽  
Bow Shock ◽  
Ion Flow ◽  
Current Sheets ◽  
The Earth ◽  
Outflow Region

<p>Satellite observations with high-resolution measurements have demonstrated the existence of intermittent current sheets and occurrence of magnetic reconnection in a quasi-parallel magnetosheath behind the terrestrial bow shock. In this Letter, by performing a three-dimensional (3-D) global hybrid simulation, we investigated the characteristics of the quasi-parallel magnetosheath of the bow shock, which is formed due to the interaction of the solar wind with the earth’s magnetosphere. Current sheets with widths of several ion inertial lengths are found to be produced in the magnetosheath after the upstream large amplitude electromagnetic waves penetrate through the shock and are then compressed in the downstream. Magnetic reconnection consequently occurs in these current sheets, where high-speed ion flow jets are identified in the outflow region. Simultaneously, flux ropes with the extension (along the   direction) of about several earth’s radii are also observed. Our simulation shed new insight on the mechanism for the occurrence of magnetic reconnection in the quasi-parallel shocked magnetosheath.</p>

Manifestation of magnetic reconnection in coronal streamer current sheets

1994 ◽  
Vol 70 (1-2) ◽  
pp. 299-302 ◽  
Author(s):  
A. I. Verneta ◽  
E. Antonucci ◽  
D. Marocchi
Keyword(s):  
Magnetic Reconnection ◽  
Current Sheets ◽  
Coronal Streamer

scholarly journals Computer studies of the three-dimensional magnetic reconnection with the superimposedBycomponent

2000 ◽  
Vol 105 (A3) ◽  
pp. 5529-5540 ◽  
Author(s):  
Ensang Lee ◽  
Kyoung-Wook Min ◽  
Jongho Seon ◽  
L. C. Lee ◽  
Dongsu Ryu
Keyword(s):  
Magnetic Reconnection ◽  
Three Dimensional ◽  
Computer Studies
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