The evolution of Alfvénic perturbations in a three-dimensional MHD model of the inner heliospheric current sheet region

1996 ◽  
Vol 101 (A12) ◽  
pp. 27603-27623 ◽  
Author(s):  
T. Stribling ◽  
D. A. Roberts ◽  
M. L. Goldstein
Keyword(s):  
Current Sheet ◽  
Three Dimensional ◽  
Heliospheric Current Sheet ◽  
Mhd Model

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.

An MHD model for a heliospheric current sheet

2004 ◽  
Vol 48 (5) ◽  
pp. 433-438 ◽  
Author(s):  
I. M. Podgorny ◽  
A. I. Podgorny ◽  
S. Minami ◽  
M. Morimoto
Keyword(s):  
Current Sheet ◽  
Heliospheric Current Sheet ◽  
Mhd Model

THREE-DIMENSIONAL WAVY HELIOSPHERIC CURRENT SHEET DRIFTS

2011 ◽  
Vol 744 (2) ◽  
pp. 170 ◽  
Author(s):  
C. Pei ◽  
J. W. Bieber ◽  
R. A. Burger ◽  
J. Clem
Keyword(s):  
Current Sheet ◽  
Three Dimensional ◽  
Heliospheric Current Sheet

scholarly journals The role of streamers in the deflection of coronal mass ejections

2011 ◽  
Vol 7 (S286) ◽  
pp. 134-138
Author(s):  
F. P. Zuccarello ◽  
A. Bemporad ◽  
C. Jacobs ◽  
M. Mierla ◽  
S. Poedts ◽  
...  
Keyword(s):  
Current Sheet ◽  
Three Dimensional ◽  
Heliospheric Current Sheet ◽  
Field Of View ◽  
Physical Explanation ◽  
Filament Eruption ◽  
Mhd Simulations ◽  
Radial Evolution ◽  
Mass Ejection

AbstractOn 2009 September 21, a filament eruption and the associated Coronal Mass Ejection (CME) was observed by the STEREO spacecraft. The CME originated from the southern hemisphere and showed a deflection of about 15° towards the heliospheric current sheet (HCS) during its propagation in the COR1 field-of-view (FOV). The aim of this paper is to provide a physical explanation for the strong deflection of the CME. We first use the STEREO observations in order to reconstruct the three dimensional (3D) trajectory of the CME. Starting from a magnetic configuration that closely resembles the potential field extrapolation for that date, we performed numerical magneto-hydrodynamics (MHD) simulations. By applying localized shearing motions, a CME is initiated in the simulation, showing a similar non-radial evolution, structure, and velocity as the observed event. The CME gets deflected towards the current sheet of the larger northern helmet streamer, due to an imbalance in the magnetic pressure and tension forces and finally it gets into the streamer and propagates along the heliospheric current sheet.

The three-dimensional geometry of the heliospheric current sheet

1985 ◽  
Vol 33 (8) ◽  
pp. 915-923 ◽  
Author(s):  
C.D. Fry ◽  
S.-I. Akasofu ◽  
J.T. Hoeksema ◽  
K. Hakamada
Keyword(s):  
Current Sheet ◽  
Three Dimensional ◽  
Heliospheric Current Sheet

scholarly journals Three-dimensional simulations of sheared current sheets: transition to turbulence?

2017 ◽  
Vol 83 (1) ◽  
Author(s):  
Imogen Gingell ◽  
Luca Sorriso-Valvo ◽  
David Burgess ◽  
Gaetano de Vita ◽  
Lorenzo Matteini
Keyword(s):  
Current Sheet ◽  
Initial Period ◽  
Three Dimensional ◽  
Power Spectra ◽  
Heliospheric Current Sheet ◽  
Transition To Turbulence ◽  
Current Sheets ◽  
Inverse Cascade ◽  
Developed Turbulence ◽  
Three Dimensional Simulations

Systems of multiple current sheets arise in various situations in natural plasmas, such as at the heliospheric current sheet in the solar wind and in the outer heliosphere in the heliosheath. Previous three-dimensional simulations have shown that such systems can develop turbulent-like fluctuations resulting from a forward and inverse cascade in wave vector space. We present a study of the transition to turbulence of such multiple current sheet systems, including the effects of adding a magnetic guide field and velocity shears across the current sheets. Three-dimensional hybrid simulations are performed of systems with eight narrow current sheets in a triply periodic geometry. We carry out a number of different analyses of the evolution of the fluctuations as the initially highly ordered state relaxes to one which resembles turbulence. Despite the evidence of a forward and inverse cascade in the fluctuation power spectra, we find that none of the simulated cases have evidence of intermittency after the initial period of fast reconnection associated with the ion tearing instability at the current sheets. Cancellation analysis confirms that the simulations have not evolved to a state which can be identified as fully developed turbulence. The addition of velocity shears across the current sheets slows the evolution in the properties of the fluctuations, but by the end of the simulation they are broadly similar. However, if the simulation is constrained to be two-dimensional, differences are found, indicating that fully three-dimensional simulations are important when studying the evolution of an ordered equilibrium towards a turbulent-like state.

Ripples in the Heliospheric Current Sheet: Dependence on Latitude and Transient Outflows

2021 ◽  
Author(s):  
Ronan Laker ◽  
Timothy Horbury ◽  
Lorenzo Matteini ◽  
Thomas Woolley ◽  
Lloyd Woodham ◽  
...  
Keyword(s):  
Solar Wind ◽  
Current Sheet ◽  
Wind Velocity ◽  
Solar Wind Velocity ◽  
Three Dimensional ◽  
Heliospheric Current Sheet ◽  
Magnetic Polarity ◽  
Magnetic Clouds ◽  
Magnetic Structures ◽  
Interaction Regions

<p>The recent launches of Parker Solar Probe (PSP), Solar Orbiter (SO) and BepiColombo, along with several legacy spacecraft, have provided the opportunity to study the solar wind at multiple latitudes and distances from the Sun simultaneously. We take advantage of this unique spacecraft constellation, along with low solar activity between May and July 2020, to investigate how latitude affects the solar wind and Heliospheric Current Sheet (HCS) structure. We use ballistic mapping to compare polarity and solar wind velocity between several spacecraft, showing that fine scale ripples in the HCS can be resolved down to several degrees in longitude. We show that considering solar wind velocity is also useful when investigating the HCS structure, as it can reveal times when the spacecraft is within slow, dense streamer belt wind without changing magnetic polarity. We measured the local orientation of planar magnetic structures associated with HCS crossings, finding that these were broadly consistent with the shape of the HCS but at much steeper angles due to compression from stream interaction regions. We identified several transient magnetic clouds associated with HCS crossings, and have shown that these can disrupt the local HCS orientation up to four days after their passage, but did not significantly affect the position of the HCS. This work highlights that the heliosphere should always be treated as three-dimensional, especially at solar minimum, where a few degrees in latitude can create a considerable difference in solar wind conditions.</p>

scholarly journals MHD simulation of the three-dimensional structure of the heliospheric current sheet

2001 ◽  
Vol 376 (1) ◽  
pp. 288-291 ◽  
Author(s):  
P. L. Israelevich ◽  
T. I. Gombosi ◽  
A. I. Ershkovich ◽  
K. C. Hansen ◽  
C. P. T. Groth ◽  
...  
Keyword(s):  
Current Sheet ◽  
Three Dimensional ◽  
Heliospheric Current Sheet ◽  
Dimensional Structure ◽  
Mhd Simulation ◽  
Three Dimensional Structure
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