Three-dimensional MHD simulation of the solar wind interaction with the ionosphere of Venus: Results of two-component reacting plasma simulation

1997 ◽  
Vol 102 (A9) ◽  
pp. 19805-19821 ◽  
Author(s):  
T. Tanaka ◽  
K. Murawski
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Plasma Simulation ◽  
Solar Wind Interaction ◽  
Mhd Simulation ◽  
Two Component

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 Full compressible 3D MHD simulation of solar wind

2020 ◽  
Vol 500 (4) ◽  
pp. 4779-4787
Author(s):  
Takuma Matsumoto
Keyword(s):  
Solar Wind ◽  
Transition Region ◽  
Solar Physics ◽  
Mass Loss Rate ◽  
Three Dimensional ◽  
Lower Atmosphere ◽  
Fast Solar Wind ◽  
Solar Mass ◽  
Mhd Simulation ◽  
Driving Mechanisms

ABSTRACT Identifying the heating mechanisms of the solar corona and the driving mechanisms of solar wind are key challenges in understanding solar physics. A full three-dimensional compressible magnetohydrodynamic (MHD) simulation was conducted to distinguish between the heating mechanisms in the fast solar wind above the open field region. Our simulation describes the evolution of the Alfvénic waves, which includes the compressible effects from the photosphere to the heliospheric distance s of 27 solar radii (R⊙). The hot corona and fast solar wind were reproduced simultaneously due to the dissipation of the Alfvén waves. The inclusion of the transition region and lower atmosphere enabled us to derive the solar mass-loss rate for the first time by performing a full three-dimensional compressible MHD simulation. The Alfvén turbulence was determined to be the dominant heating mechanism in the solar wind acceleration region (s &gt; 1.3 R⊙), as suggested by previous solar wind models. In addition, shock formation and phase mixing are important below the lower transition region (s &lt; 1.03 R⊙) as well.

A three-dimensional MHD simulation of the interaction of the solar wind with comet Halley

1988 ◽  
Vol 93 (A9) ◽  
pp. 9568 ◽  
Author(s):  
Tatsuki Ogino ◽  
Raymond J. Walker ◽  
Maha Ashour-Abdalla
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Mhd Simulation ◽  
Comet Halley
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