Three-dimensional hybrid simulation of magnetosheath reconnection under northward and southward interplanetary magnetic field

2010 ◽  
Vol 115 (A3) ◽  
pp. n/a-n/a ◽  
Author(s):  
Y. Pang ◽  
Y. Lin ◽  
X. H. Deng ◽  
X. Y. Wang ◽  
B. Tan
Keyword(s):  
Magnetic Field ◽  
Interplanetary Magnetic Field ◽  
Three Dimensional ◽  
Hybrid Simulation

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.

Mercury’s magnetosphere–solar wind interaction for northward and southward interplanetary magnetic field: Hybrid simulation results

Icarus ◽  
2010 ◽  
Vol 209 (1) ◽  
pp. 11-22 ◽  
Author(s):  
Pavel M. Trávníček ◽  
David Schriver ◽  
Petr Hellinger ◽  
David Herčík ◽  
Brian J. Anderson ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Hybrid Simulation ◽  
Solar Wind Interaction ◽  
Simulation Results

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 Three-dimensional MHD simulation of interplanetary magnetic field changes at 1 AU as a consequence of simulated solar flares

1996 ◽  
Vol 14 (4) ◽  
pp. 383-399 ◽  
Author(s):  
C.-C. Wu ◽  
M. Dryer ◽  
S. T. Wu
Keyword(s):  
Magnetic Field ◽  
Solar Activity ◽  
Interplanetary Magnetic Field ◽  
Pressure Pulse ◽  
Initial Conditions ◽  
Three Dimensional ◽  
Strong Relationship ◽  
Heliospheric Current Sheet ◽  
Archimedean Spiral ◽  
The North

Abstract. A fully three-dimensional (3D), time-dependent, MHD interplanetary global model (3D IGM) has been used, for the first time, to study the relationship between different forms of solar activity and transient variations of the north-south component, Bz, of the interplanetary magnetic field (IMF) at 1 AU. One form of solar activity, the flare, is simulated by using a pressure pulse at different locations near the solar surface and observing the simulated IMF evolution of Bθ (=–Bz) at 1 AU. Results show that, for a given pressure pulse, the orientation of the corresponding transient variation of Bz has a strong relationship to the location of the pressure pulse and the initial conditions of the IMF. Two initial IMF conditions are considered: a unipolar Archimedean spiral with outward polarity and a flat heliospheric current sheet (HCS) with outward polarity in the northern hemisphere and which gradually reverses polarity in the solar equatorial plane to inward polarity in the southern heliospheric hemisphere. The wave guide effect of the HCS is also demonstrated.

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