The Large-Scale Density Structure of the Solar Corona and the Heliospheric Current Sheet

1996 ◽  
Vol 458 ◽  
pp. 817 ◽  
Author(s):  
Madhulika Guhathakurta ◽  
Thomas E. Holzer ◽  
R. M. MacQueen
Keyword(s):  
Solar Corona ◽  
Current Sheet ◽  
Large Scale ◽  
Heliospheric Current Sheet ◽  
Density Structure

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.

Photometrical Evidences in Favour of the “Flat Solar Corona”

1994 ◽  
Vol 144 ◽  
pp. 111-113
Author(s):  
R. A. Gulyaev ◽  
N. Ya. Vanyarkha ◽  
E. S. Vanyarkha
Keyword(s):  
Solar Corona ◽  
Current Sheet ◽  
Physical Meaning ◽  
Quantitative Description ◽  
Sunspot Cycle ◽  
Standard Technique ◽  
Heliospheric Current Sheet ◽  
Frame Of Reference ◽  
Clear Physical Meaning ◽  
Conventional View

AbstractThe conventional way of quantitative description of coronal forms is shown to be inadequate as compared with actual coronal configurations. The standard technique of determining the Ludendorff’s parameter in the heiiographic reference has no physical meaning. However the similar parameter as determined in the heliomagnetic frame of reference is of quite clear physical meaning since it depicts the actual concentration of the coronal material towards the heliospheric current sheet. Conclusion of a need to revise the conventional view on relation of coronal forms with the sunspot cycle is pointed out.

Phenomenological Pattern of the Outer Solar Corona Structure

1994 ◽  
Vol 144 ◽  
pp. 115-117
Author(s):  
R. A. Gulyaev
Keyword(s):  
Solar Corona ◽  
Current Sheet ◽  
3D Structure ◽  
Heliospheric Current Sheet ◽  
Hyperbolic Paraboloid ◽  
Corona Structure ◽  
Outer Corona ◽  
Second Degree

AbstractTopology of the outer solar corona has been analysed. In doing so the outer corona is treated as a visible manifestation of the heliospheric current sheet base. Generalization of the recent conception of the flat (galaxy-like) solar corona has been suggested. It is shown that 3D structure of the outer corona is well fitted by a second-degree surface of a hyperbolic paraboloid.

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