Magnetic reconnection in the presence of sheared plasma flow: Intermediate shock formation

1994 ◽  
Vol 1 (3) ◽  
pp. 706-713 ◽  
Author(s):  
A. L. La Belle‐Hamer ◽  
A. Otto ◽  
L. C. Lee
Keyword(s):  
Magnetic Reconnection ◽  
Plasma Flow ◽  
Shock Formation ◽  
Intermediate Shock

scholarly journals Effect of interchange instability on magnetic reconnection

2013 ◽  
Vol 20 (3) ◽  
pp. 365-377 ◽  
Author(s):  
W. Lyatsky ◽  
M. L. Goldstein
Keyword(s):  
Magnetic Fields ◽  
Electric Field ◽  
Magnetic Reconnection ◽  
Plasma Flow ◽  
Buoyancy Force ◽  
Strong Turbulence ◽  
Polarization Electric Field ◽  
Interchange Instability ◽  
Reconnection Layer ◽  
Fast Reconnection

Abstract. We present here the results of a study of interacting magnetic fields that involves a force normal to the reconnection layer. In the presence of such force, the reconnection layer becomes unstable to interchange disturbances. The interchange instability results in formation of tongues of heated plasma that leaves the reconnection layer through its wide surface rather than through its narrow ends, as is the case in traditional magnetic reconnection models. This plasma flow out of the reconnection layer facilitates the removal of plasma from the layer and leads to fast reconnection. The proposed mechanism provides fast reconnection of interacting magnetic fields and does not depend on the thickness of the reconnection layer. This instability explains the strong turbulence and bidirectional streaming of plasma that is directed toward and away from the reconnection layer that is observed frequently above reconnection layers. The force normal to the reconnection layer also accelerates the removal of plasma islands appearing in the reconnection layer during turbulent reconnection. In the presence of this force normal to the reconnection layer, these islands are removed from the reconnection layer by the "buoyancy force", as happens in the case of interchange instability that arises due to the polarization electric field generated at the boundaries of the islands.

scholarly journals Magnetically Driven Motions in Solar Corona

1980 ◽  
Vol 91 ◽  
pp. 487-489 ◽  
Author(s):  
B. V. Somov ◽  
S. I. Syrovatskii
Keyword(s):  
Magnetic Field ◽  
Solar Corona ◽  
Magnetic Reconnection ◽  
Current Sheet ◽  
Magnetic Dipole ◽  
Plasma Flow ◽  
Strong Field ◽  
Plasma Velocity ◽  
Rapid Process

Solution of the nonlinear MHD problem of plasma flow in an increasing dipolar magnetic field is obtained in the approximation of a strong field. The distributions of plasma velocity, displacement, and density are calculated. The situation when the magnetic dipole is ‘increased’ by rapid process of magnetic reconnection or current sheet rupture is illustrated. Possible applications are discussed in connection with plasma ejections from chromosphere in corona.

scholarly journals Summary of Conference

1985 ◽  
Vol 107 ◽  
pp. 529-536
Author(s):  
Vytenis M. Vasyliunas
Keyword(s):  
Magnetic Field ◽  
Electric Field ◽  
Magnetic Reconnection ◽  
Field Line ◽  
Magnetic Field Line ◽  
Plasma Flow ◽  
Remarkable Degree ◽  
Ideal Mhd ◽  
Points Of View ◽  
The Magnetic Field

For a meeting of people from such widely different fields, this Symposium has exhibited a remarkable degree of unity. There has been one key concept running as a thread throughout the Symposium: the concept of magnetic field line reconnection, or magnetic field line merging as I prefer to call it. It was dealt with directly in many papers, and many others dealt indirectly with it and various related aspects. The concept was applied in the Symposium to an amazing variety of objects and was examined from many points of view and by many different techniques. Magnetic field line reconnection or merging is a paradoxical concept. It clearly depends upon magnetohydrodynamics (MHD); for example, constraints imposed by the MHD relation between the magnetic field and the plasma flow are essential to set it up - without these constraints (if, for example, the electric field parallel to the magnetic field could assume any desired value) the problems we discuss under the heading of magnetic reconnection would merely be moderately complicated problems of magnetostatics. At the same time, departures from ideal MHD are also an essential and unavoidable part of the concept.

scholarly journals Numerical Simulation of the Explosive Events in the Solar Atmosphere

1993 ◽  
Vol 141 ◽  
pp. 134-137
Author(s):  
Shu-Ping Jiu
Keyword(s):  
Numerical Simulation ◽  
Magnetic Flux ◽  
Magnetic Reconnection ◽  
Solar Atmosphere ◽  
Plasma Flow ◽  
Small Scale ◽  
Flare Activity ◽  
Specific Location ◽  
Mhd Simulations ◽  
Explosive Events

AbstractExplosive events are the earliest indicators of flare activity and potentially predict the imminent occurrence of a flare at a specific location. They are highly energetic small-scale phenomena which are frequently detected throughout the quiet and active sun. The observations show that explosive events are related to emerging magnetic flux and tend to occur on the edges of high photospheric magnentic field regions. The cancellation of photospheric magnetic flux are the manifestation of explosive events, so that they are identified as the magnetic reconnection of flux elements. We assume that emerging flux are convected to the network boundaries with the typical velocity of intranetwork elements. Two-dimension (2D) compressible MHD simulations are performed to explore the reconnection process between emerging intranework flux and network field. The numerical results clearly show the cancellation of magnetic flux and the acceleration of the plasma flow.

OBSERVATIONS OF AN INTERPLANETARY INTERMEDIATE SHOCK ASSOCIATED WITH A MAGNETIC RECONNECTION EXHAUST

2016 ◽  
Vol 826 (1) ◽  
pp. 15 ◽  
Author(s):  
H. Q. Feng ◽  
Q. H. Li ◽  
J. M. Wang ◽  
G. Q. Zhao
Keyword(s):  
Magnetic Reconnection ◽  
Intermediate Shock

Interaction between plasma flow and a magnetic barrier: shock formation

1968 ◽  
Vol 8 (4) ◽  
pp. 362-364 ◽  
Author(s):  
C. Leloup ◽  
R.T. Taussig
Keyword(s):  
Plasma Flow ◽  
Shock Formation ◽  
Magnetic Barrier

scholarly journals Magnetic field generation, Weibel-mediated collisionless shocks, and magnetic reconnection in colliding laser-produced plasmas

2015 ◽  
Vol 11 (A29A) ◽  
pp. 329-332
Author(s):  
W. Fox ◽  
A. Bhattacharjee ◽  
G. Fiksel
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Magnetic Reconnection ◽  
Magnetic Energy ◽  
Cosmic Ray ◽  
Laboratory Astrophysics ◽  
Shock Acceleration ◽  
Shock Formation ◽  
Magnetic Field Generation ◽  
Temperature Plasma

AbstractColliding plasmas are ubiquitous in astrophysical environments and allow conversion of kinetic energy into heat and, most importantly, the acceleration of particles to extremely high energies to form the cosmic ray spectrum. In collisionless astrophysical plasmas, kinetic plasma processes govern the interaction and particle acceleration processes, including shock formation, self-generation of magnetic fields by kinetic plasma instabilities, and magnetic field compression and reconnection. How each of these contribute to the observed spectra of cosmic rays is not fully understood, in particular both shock acceleration processes and magnetic reconnection have been proposed. We will review recent results of laboratory astrophysics experiments conducted at high-power, inertial-fusion-class laser facilities, which have uncovered significant results relevant to these processes. Recent experiments have now observed the long-sought Weibel instability between two interpenetrating high temperature plasma plumes, which has been proposed to generate the magnetic field necessary for shock formation in unmagnetized regimes. Secondly, magnetic reconnection has been studied in systems of colliding plasmas using either self-generated magnetic fields or externally applied magnetic fields, and show extremely fast reconnection rates, indicating fast destruction of magnetic energy and further possibilities to accelerate particles. Finally, we highlight kinetic plasma simulations, which have proven to be essential tools in the design and interpretation of these experiments.

scholarly journals Slow shock formation and structure with sub-Alfvénic shear flow in magnetic reconnection

2012 ◽  
Vol 117 (A6) ◽  
pp. n/a-n/a ◽  
Author(s):  
L. J. Li ◽  
X. Zhang ◽  
L. C. Wang ◽  
Z. W. Ma
Keyword(s):  
Shear Flow ◽  
Magnetic Reconnection ◽  
Shock Formation ◽  
Slow Shock
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