Effects of a guide field on the evolution of a current sheet

2006 ◽  
Vol 13 (10) ◽  
pp. 102902 ◽  
Author(s):  
C. L. Tsai ◽  
L. C. Lee ◽  
B. H. Wu
Keyword(s):  
Current Sheet ◽  
Guide Field ◽  
A Current

Gyrokinetic theory of electrostatic lower-hybrid drift instabilities in a current sheet with guide field

2014 ◽  
Vol 21 (5) ◽  
pp. 052104 ◽  
Author(s):  
K. Tummel ◽  
L. Chen ◽  
Z. Wang ◽  
X. Y. Wang ◽  
Y. Lin
Keyword(s):  
Current Sheet ◽  
Lower Hybrid ◽  
Guide Field ◽  
A Current

Estimation of electromagnetic field in air by a magnetic dipole in the sea based on a current sheet model

2016 ◽  
Vol 10 (7) ◽  
pp. 709-718
Author(s):  
Honglei Wang ◽  
Kunde Yang ◽  
Kun Zheng ◽  
Yixin Yang ◽  
Yuanliang Ma
Keyword(s):  
Electromagnetic Field ◽  
Current Sheet ◽  
Magnetic Dipole ◽  
A Current

Propagation of a shock wave across a current sheet without reflection

2017 ◽  
Vol 52 (4) ◽  
pp. 463-467 ◽  
Author(s):  
S. D. Kovalevskaya
Keyword(s):  
Shock Wave ◽  
Current Sheet ◽  
A Current

Statistics on Jupiter's Current Sheet with Juno Data: Geometry, Magnetic Fields and Energetic Particles

2021 ◽  
Author(s):  
Zhi-Yang Liu ◽  
Qiu-Gang Zong ◽  
Michel Blanc
Keyword(s):  
Magnetic Fields ◽  
Current Sheet ◽  
Power Law ◽  
Heavy Ions ◽  
Particle Interaction ◽  
The Other ◽  
Gaussian Functions ◽  
Fixed Energy ◽  
Thin Current Sheet ◽  
A Current

<p>Jupiter's magnetosphere contains a current sheet of huge size near its equator. The current sheet not only mediates the global mass and energy cycles of Jupiter's magnetosphere, but also provides an occurring place for many localized dynamic processes, such as reconnection and wave-particle interaction. To correctly evaluate its role in these processes, a statistical description of the current sheet is required. To this end, here we conduct statistics on Jupiter's current sheet, with four-year Juno data recorded in the 20-100 Jupiter radii, post-midnight magnetosphere. The results suggest a thin current sheet whose thickness is comparable with the gyro-radius of dominant ions. Magnetic fields in the current sheet decrease in power-law with increasing radial distances. At fixed energy, the flux of electrons and protons increases with decreasing radial distances. On the other hand, at fixed radial distances, the flux decreases in power-law with increasing energy. The flux also varies with the distances to the current sheet center. The corresponding relationship can be well described by Gaussian functions peaking at the current sheet center. In addition, the statistics show the flux of oxygen- and sulfur-group ions is comparable with the flux of protons at the same energy and radial distances, indicating the non-negligible effects of heavy ions on current sheet dynamics. From these results, a statistical model of Jupiter's current sheet is constructed, which provides us with a start point of understanding the dynamics of the whole Jupiter's magnetosphere.</p>

scholarly journals Rapid dissipation in a current sheet driven by footpoints motions

2006 ◽  
Vol 458 (1) ◽  
pp. 307-315
Author(s):  
G. Fruit ◽  
I. J. D. Craig
Keyword(s):  
Current Sheet ◽  
A Current

scholarly journals 3D turbulent reconnection driven current-sheet dynamics: solar applications

2010 ◽  
Vol 6 (S274) ◽  
pp. 458-460
Author(s):  
Lapo Bettarini ◽  
Giovanni Lapenta
Keyword(s):  
Current Sheet ◽  
Characteristic Time ◽  
Three Dimensional ◽  
Reynolds Numbers ◽  
Anomalous Effect ◽  
Instability Modes ◽  
Diffusive Dynamics ◽  
Three Dimensional Configuration ◽  
A Current ◽  
Dimensional Picture

AbstractWe provide a complete three-dimensional picture of the reconnecting dynamics of a current-sheet. Recently, a two-dimensional non-steady reconnection dynamics has been proved to occur without the presence of any anomalous effect (Lapenta, 2008, Skender & Lapenta, 2010, Bettarini & Lapenta, 2010) but such a picture must be confirmed in a full three-dimensional configuration wherein all instability modes are allowed to drive the evolution of the system, i.e. to sustain a reconnection dynamics or to push the system along a different instability path. Here we propose a full-space analysis allowing us to determine the longitudinal and, possibly, the transversal modes driving the different current-sheet disruption regimes, the corresponding characteristic time-scales and to study system's instability space- parameter (plasma beta, Lundquist and Reynolds numbers, system's aspect ratio). The conditions leading to an explosive evolution rather then to a diffusive dynamics as well as the details of the reconnection inflow/outflow regime at the disruption phase are determined. Such system embedded in a solar-like environment and undergoing a non-steady reconnection evolution may determine the formation both of jets and waves influencing the dynamics and energetic of the upper layers and of characteristic down-flows as observed in the low solar atmosphere.

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