Two-dimensional Magnetohydrodynamic Simulations of Relativistic Magnetic Reconnection

2006 ◽  
Vol 647 (2) ◽  
pp. L123-L126 ◽  
Author(s):  
Naoyuki Watanabe ◽  
Takaaki Yokoyama
Keyword(s):  
Magnetic Reconnection ◽  
Two Dimensional ◽  
Magnetohydrodynamic Simulations

Kinetic Alfvén Waves Excited in Two-Dimensional Magnetic Reconnection

2018 ◽  
Vol 123 (8) ◽  
pp. 6655-6669 ◽  
Author(s):  
Hongtao Huang ◽  
Yiqun Yu ◽  
Lei Dai ◽  
Tieyan Wang
Keyword(s):  
Magnetic Reconnection ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Two Dimensional ◽  
Kinetic Alfvén Waves

MAGNETIC FIELD AMPLIFICATION BY RELATIVISTIC SHOCKS IN AN INHOMOGENEOUS MEDIUM

2012 ◽  
Vol 08 ◽  
pp. 364-367
Author(s):  
YOSUKE MIZUNO ◽  
MARTIN POHL ◽  
JACEK NIEMIEC ◽  
BING ZHANG ◽  
KEN-ICHI NISHIKAWA ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Inhomogeneous Medium ◽  
Magnetic Energy ◽  
Small Scale ◽  
Two Dimensional ◽  
Filamentary Structure ◽  
Field Amplification ◽  
Relativistic Shocks ◽  
Field Lines ◽  
Magnetohydrodynamic Simulations

We perform two-dimensional relativistic magnetohydrodynamic simulations of a mildly relativistic shock propagating through an inhomogeneous medium. We show that the postshock region becomes turbulent owing to preshock density inhomogeneity, and the magnetic field is strongly amplified due to the stretching and folding of field lines in the turbulent velocity field. The amplified magnetic field evolves into a filamentary structure in two-dimensional simulations. The magnetic energy spectrum is flatter than the Kolmogorov spectrum and indicates that the so-called small-scale dynamo is occurring in the postshock region. We also find that the amplitude of magnetic-field amplification depends on the direction of the mean preshock magnetic field.

scholarly journals Two-dimensional Radiative Magnetohydrodynamic Simulations of Partial Ionization in the Chromosphere. II. Dynamics and Energetics of the Low Solar Atmosphere

2017 ◽  
Vol 847 (1) ◽  
pp. 36 ◽  
Author(s):  
Juan Martínez-Sykora ◽  
Bart De Pontieu ◽  
Mats Carlsson ◽  
Viggo H. Hansteen ◽  
Daniel Nóbrega-Siverio ◽  
...  
Keyword(s):  
Solar Atmosphere ◽  
Two Dimensional ◽  
Magnetohydrodynamic Simulations

scholarly journals Magnetic Reconnection with Sweet-Parker Characteristics in Two-dimensional Laboratory Plasmas

10.2172/3001 ◽  
1999 ◽  
Author(s):  
T. Carter ◽  
S. Hsu ◽  
H. Ji ◽  
R. Kulsrud ◽  
M. Yamada ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Two Dimensional ◽  
Laboratory Plasmas

scholarly journals Quasi-separatrix Layers Induced by Ballooning Instability in Near-Earth Magnetotail

2019 ◽  
Author(s):  
Ping Zhu ◽  
Zechen Wang ◽  
Jun Chen ◽  
Xingting Yan ◽  
Rui Liu
Keyword(s):  
Numerical Simulations ◽  
Magnetic Reconnection ◽  
Solar Physics ◽  
Close Correlation ◽  
Satellite Observations ◽  
Two Dimensional ◽  
3 Dimensional ◽  
Ballooning Instability ◽  
3D Geometry ◽  
Alternative Means

Abstract. Magnetic reconnection processes in the near-Earth magnetotail can be highly 3-dimensional (3D) in geometry and dynamics, even though the magnetotail configuration itself is nearly two dimensional due to the symmetry in the dusk-dawn direction. Such reconnection processes can be induced by the 3D dynamics of nonlinear ballooning instability. In this work, we explore the global 3D geometry of the reconnection process induced by ballooning instability in the near-Earth magnetotail by examining the distribution of quasi-separatrix layers associated with plasmoid formation in the entire 3D domain of magnetotail configuration, using an algorithm previously developed in context of solar physics. The 3D distribution of quasi-separatrix layers (QSLs) as well as their evolution directly follows the plasmoid formation during the nonlinear development of ballooning instability in both time and space. Such a close correlation demonstrates a strong coupling between the ballooning and the corresponding reconnection processes. It further confirms the intrinsic 3D nature of the ballooning-induced plasmoid formation and reconnection processes, in both geometry and dynamics. In addition, the reconstruction of the 3D QSL geometry may provide an alternative means for identifying the location and timing of 3D reconnection sites in magnetotail from both numerical simulations and satellite observations.

Orientation of the X-line in asymmetric magnetic reconnection

2016 ◽  
Vol 82 (4) ◽  
Author(s):  
N. Aunai ◽  
M. Hesse ◽  
B. Lavraud ◽  
J. Dargent ◽  
R. Smets
Keyword(s):  
Magnetic Reconnection ◽  
Domain Size ◽  
Shear Angle ◽  
Two Dimensional ◽  
Field Profile ◽  
Reconnection Rate ◽  
Magnetic Shear ◽  
Magnetic Field Profile ◽  
The Earth ◽  
Set Up

Magnetic reconnection can occur in current sheets separating magnetic fields sheared by any angle and of arbitrarily different amplitudes. In such asymmetric and non-coplanar systems, it is not yet understood what the orientation of the X-line will be. Studying how this orientation is determined locally by the reconnection process is important to understand systems such as the Earth magnetopause, where reconnection occurs in regions with large differences in upstream plasma and field properties. This study aims at determining what the local X-line orientation is for different upstream magnetic shear angles in an asymmetric set-up relevant to the Earth’s magnetopause. We use two-dimensional hybrid simulations and vary the simulation plane orientation with regard to the fixed magnetic field profile and search for the plane maximizing the reconnection rate. We find that the plane defined by the bisector of upstream fields maximizes the reconnection rate and this appears not to depend on the magnetic shear angle, domain size or upstream plasma and asymmetries.

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