scholarly journals Three-dimensional MHD simulations of the steady state magnetosphere with northward interplanetary magnetic field

2001 ◽  
Vol 106 (A1) ◽  
pp. 275-287 ◽  
Author(s):  
P. N. Guzdar ◽  
X. Shao ◽  
C. C. Goodrich ◽  
K. Papadopoulos ◽  
M. J. Wiltberger ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Steady State ◽  
Interplanetary Magnetic Field ◽  
Three Dimensional ◽  
Mhd Simulations

scholarly journals Coronal energy release by MHD avalanches: continuous driving

2018 ◽  
Vol 615 ◽  
pp. A84 ◽  
Author(s):  
J. Reid ◽  
A. W. Hood ◽  
C. E. Parnell ◽  
P. K. Browning ◽  
P. J. Cargill
Keyword(s):  
Magnetic Field ◽  
Steady State ◽  
Coronal Loop ◽  
Magnetic Energy ◽  
Three Dimensional ◽  
Mhd Simulations ◽  
First Time ◽  
Viable Mechanism ◽  
The Magnetic Field ◽  
Heating Profile

Previous work has confirmed the concept of a magnetohydrodynamic (MHD) avalanche in pre-stressed threads within a coronal loop. We undertook a series of full, three-dimensional MHD simulations in order to create three threads by twisting the magnetic field through boundary motions until an instability ensues. We find that, following the original instability, one unstable thread can disrupt its neighbours with continued driving. A “bursty” heating profile results, with a series of ongoing energy releases, but no evident steady state. For the first time using full MHD, we show that avalanches are a viable mechanism for the storing and release of magnetic energy in the solar corona, as a result of photospheric motions.

Three-dimensional Multispecies Simulation of the Solar Wind Interaction with Mars Under Different Interplanetary Magnetic Field Orientations

2021 ◽  
Vol 921 (2) ◽  
pp. 139
Author(s):  
Yun Li ◽  
Haoyu Lu ◽  
Jinbin Cao ◽  
Shibang Li ◽  
Christian Mazelle ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Three Dimensional ◽  
Polarity Reversal ◽  
Solar Wind Interaction ◽  
Magnetic Structures ◽  
Parker Spiral ◽  
Global Configuration ◽  
Spiral Angle

Abstract Without the intrinsic magnetic field, the solar wind interaction with Mars can be significantly different from the interaction with Earth and other magnetized planets. In this paper, we investigate how a global configuration of the magnetic structures, consisting of the bow shock, the induced magnetosphere, and the magnetotail, is modulated by the interplanetary magnetic field (IMF) orientation. A 3D multispecies numerical model is established to simulate the interaction of solar wind with Mars under different IMF directions. The results show that the shock size including the subsolar distance and the terminator radius increases with Parker spiral angle, as is the same case with the magnetotail radius. The location and shape of the polarity reversal layer and inverse polarity reversal layer in the induced magnetotail are displaced to the y < 0 sector for a nonzero flow-aligned IMF component, consistent with previous analytical solutions and observations. The responses of the Martian global magnetic configuration to the different IMF directions suggest that the external magnetic field plays an important role in the solar wind interaction with unmagnetized planets.

scholarly journals High Resolution 3D Relativistic MHD Simulations of Jets

2009 ◽  
Vol 5 (H15) ◽  
pp. 254-255
Author(s):  
A. Ferrari ◽  
A. Mignone ◽  
P. Rossi ◽  
G. Bodo ◽  
S. Massaglia
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Numerical Simulations ◽  
Three Dimensional ◽  
Full Length ◽  
Toroidal Field ◽  
Toroidal Magnetic Field ◽  
Mhd Simulations ◽  
Strong Current

AbstractWe performed high-resolution three dimensional numerical simulations of relativistic MHD jets carrying an initially toroidal magnetic field responsible for the process of jet acceleration and collimation. We find that in the 3D case the toroidal field gives rise to strong current driven kink instabilities leading to jet wiggling. However, it appears to be able to maintain an highly relativistic spine along its full length.

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