Application of the catastrophe theory in studying the magnetic reconnection process

2012 ◽  
Vol 4 (2) ◽  
pp. 135-143 ◽  
Author(s):  
D. P. Kostomarov ◽  
E. Yu. Echkina ◽  
I. N. Inovenkov
Keyword(s):  
Magnetic Reconnection ◽  
Catastrophe Theory ◽  
Reconnection Process

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.

Magnetic reconnection process in transient coaxial helicity injection

2013 ◽  
Vol 20 (9) ◽  
pp. 090702 ◽  
Author(s):  
F. Ebrahimi ◽  
E. B. Hooper ◽  
C. R. Sovinec ◽  
R. Raman
Keyword(s):  
Magnetic Reconnection ◽  
Helicity Injection ◽  
Reconnection Process ◽  
Coaxial Helicity Injection

scholarly journals Achieving fast reconnection in resistive MHD models via turbulent means

2012 ◽  
Vol 19 (2) ◽  
pp. 251-263 ◽  
Author(s):  
G. Lapenta ◽  
A. Lazarian
Keyword(s):  
Theoretical Model ◽  
Magnetic Reconnection ◽  
Numerical Experiments ◽  
Numerical Evidence ◽  
Reconnection Process ◽  
Fast Reconnection ◽  
Spontaneous Onset

Abstract. Astrophysical fluids are generally turbulent and this preexisting turbulence must be taken into account for models of magnetic reconnection in astrophysical, solar or heliospheric environments. In addition, reconnection itself induces turbulence which provides an important feedback on the reconnection process. In this paper we discuss both the theoretical model and numerical evidence that magnetic reconnection becomes fast in the approximation of resistive MHD. We consider the relation between the Lazarian and Vishniac turbulent reconnection theory and Lapenta's numerical experiments testifying of the spontaneous onset of turbulent reconnection in systems which are initially laminar.

scholarly journals Phase diagrams of forced magnetic reconnection in Taylor’s model

2015 ◽  
Vol 81 (5) ◽  
Author(s):  
L. Comisso ◽  
D. Grasso ◽  
F. L. Waelbroeck
Keyword(s):  
Magnetic Reconnection ◽  
Phase Diagrams ◽  
Dynamical Evolution ◽  
Wave Number ◽  
Boundary Perturbation ◽  
Physical Systems ◽  
Reconnection Process ◽  
Magnetic Prandtl Number ◽  
Forced Magnetic Reconnection ◽  
Fast Reconnection

Recent progress in the understanding of how externally driven magnetic reconnection evolves is organized in terms of parameter space diagrams. These diagrams are constructed using four pivotal dimensionless parameters: the Lundquist number $S$, the magnetic Prandtl number $P_{m}$, the amplitude of the boundary perturbation $\hat{{\it\Psi}}_{0}$, and the perturbation wave number $\hat{k}$. This new representation highlights the parameter regions of a given system in which the magnetic reconnection process is expected to be distinguished by a specific evolution. Contrary to previously proposed phase diagrams, the diagrams introduced here take into account the dynamical evolution of the reconnection process and are able to predict slow or fast reconnection regimes for the same values of $S$ and $P_{m}$, depending on the parameters that characterize the external drive, which have not been considered until now. These features are crucial to understanding the onset and evolution of magnetic reconnection in diverse physical systems.

scholarly journals Observational Evidence for Magnetic Reconnection in Microwave Solar Bursts

1985 ◽  
Vol 107 ◽  
pp. 185-190 ◽  
Author(s):  
M. R. Kundu
Keyword(s):  
Magnetic Reconnection ◽  
Spatial Resolution ◽  
Observational Evidence ◽  
Large Array ◽  
Very Large Array ◽  
Reconnection Process ◽  
Solar Bursts

In this paper, we first discuss a set of 6 cm observations made with the NRAO Very Large Array (VLA) (spatial resolution ~ 2″) that pertain to changes in the coronal magentic field configurations that took place before the onset of an impulsive burst observed on 14 May 1980. We also discuss a second set of 6 cm VLA observations (spatial resolution 18″ arc) where several interacting loops were involved in triggering the onset of an impulsive burst observed on June 24, 1980, 19:57:00 UT. Both sets of observations are examples of magnetic reconnection process being involved in accelerating microwave emitting electrons.

scholarly journals Coronal quasi-periodic fast-propagating magnetosonic waves observed by SDO/AIA

2015 ◽  
Vol 11 (S320) ◽  
pp. 103-105
Author(s):  
Yuandeng Shen
Keyword(s):  
Magnetic Reconnection ◽  
Spatial Resolution ◽  
Solar Dynamics Observatory ◽  
Reconnection Process ◽  
Temporal And Spatial ◽  
Solar Dynamics ◽  
Physic Process

AbstractCoronal quasi-periodic fast-propagating (QFP) magnetosonic waves are scare in previous studies due to the relative low temporal and spatial resolution of past telescopes. Recently, they are detected by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). Here, two cases of QFP waves are presented. The analysis results indicate that QFP waves are tightly associated with the associated flares. It is indicate that QFP waves and the associated flares are possibly driven by the same physic process such as quasi-periodic magnetic reconnection process in producing flares.

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