scholarly journals Reply [to “Comment on “Global magnetohydrodynamic simulation of a comet crossing the heliospheric current sheet” by Y. Yi et al.”]

1998 ◽  
Vol 103 (A4) ◽  
pp. 6637-6639 ◽  
Author(s):  
Yu Yi ◽  
Raymond J. Walker ◽  
Tatsuki Ogino ◽  
John C. Brandt
Keyword(s):  
Current Sheet ◽  
Heliospheric Current Sheet ◽  
Magnetohydrodynamic Simulation

Global magnetohydrodynamic simulation of a comet crossing the heliospheric current sheet

1996 ◽  
Vol 101 (A12) ◽  
pp. 27585-27601 ◽  
Author(s):  
Yu Yi ◽  
Raymond J. Walker ◽  
Tatsuki Ogino ◽  
John C. Brandt
Keyword(s):  
Current Sheet ◽  
Heliospheric Current Sheet ◽  
Magnetohydrodynamic Simulation

Solar wind double ion beams and the heliospheric current sheet

1995 ◽  
Vol 100 (A5) ◽  
pp. 7881 ◽  
Author(s):  
C. M. Hammond ◽  
W. C. Feldman ◽  
J. L. Phillips ◽  
B. E. Goldstein ◽  
A. Balogh
Keyword(s):  
Solar Wind ◽  
Current Sheet ◽  
Heliospheric Current Sheet ◽  
Ion Beams

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.

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