scholarly journals A three-dimensional, multispecies, comprehensive MHD model of the solar wind interaction with the planet Venus

2009 ◽  
Vol 114 (A9) ◽  
pp. n/a-n/a ◽  
Author(s):  
N. Terada ◽  
H. Shinagawa ◽  
T. Tanaka ◽  
K. Murawski ◽  
K. Terada
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Solar Wind Interaction ◽  
Mhd Model

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 Numerical Study of Divergence Cleaning and Coronal Heating/Acceleration Methods in the 3D COIN-TVD MHD Model

2021 ◽  
Vol 9 ◽  
Author(s):  
Chang Liu ◽  
Fang Shen ◽  
Yousheng Liu ◽  
Man Zhang ◽  
Xiaojing Liu
Keyword(s):  
Solar Wind ◽  
Numerical Study ◽  
Three Dimensional ◽  
Coronal Heating ◽  
Solar Wind Structure ◽  
Wind Simulation ◽  
Simulation Results ◽  
Mhd Model ◽  
Cleaning Methods ◽  
Powell Method

In the solar coronal numerical simulation, the coronal heating/acceleration and the magnetic divergence cleaning techniques are very important. The coronal–interplanetary total variation diminishing (COIN-TVD) magnetohydrodynamic (MHD) model is developed in recent years that can effectively realize the coronal–interplanetary three-dimensional (3D) solar wind simulation. In this study, we focus on the 3D coronal solar wind simulation by using the COIN-TVD MHD model. In order to simulate the heating and acceleration of solar wind in the coronal region, the volume heating term in the model is improved efficiently. Then, the influence of the different methods to reduce the ∇⋅B constraint error on the coronal solar wind structure is discussed. Here, we choose Carrington Rotation (CR) 2199 as a study case and try to make a comparison of the simulation results among the different magnetic divergence cleaning methods, including the diffusive method, the Powell method, and the composite diffusive/Powell method, by using the 3D COIN-TVD MHD model. Our simulation results show that with the different magnetic divergence cleaning methods, the ∇⋅B error can be reduced in different levels during the solar wind simulation. Among the three divergence cleaning methods we used, the composite diffusive/Powell method can maintain the divergence cleaning constraint better to a certain extent, and the relative magnetic field divergence error can be controlled in the order of 10−9. Although these numerical simulations are performed for the background solar corona, these methods are also suitable for the simulation of CME initiation and propagation.

scholarly journals A two-dimensional MHD model of the solar wind interaction with Mars

1999 ◽  
Vol 51 (1) ◽  
pp. 55-60 ◽  
Author(s):  
H. Shinagawa ◽  
S. W. Bougher
Keyword(s):  
Solar Wind ◽  
Two Dimensional ◽  
Solar Wind Interaction ◽  
Mhd Model

Three-dimensional simulations of the solar wind interaction with Mars

1993 ◽  
Vol 98 (A2) ◽  
pp. 1345-1357 ◽  
Author(s):  
Stephen H. Brecht ◽  
John R. Ferrante ◽  
J. G. Luhmann
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Solar Wind Interaction ◽  
Three Dimensional Simulations

scholarly journals Ultra-low-frequency waves in the ion foreshock of Mercury: a global hybrid modelling study

2019 ◽  
Vol 491 (3) ◽  
pp. 4147-4161 ◽  
Author(s):  
R Jarvinen ◽  
M Alho ◽  
E Kallio ◽  
T I Pulkkinen
Keyword(s):  
Solar Wind ◽  
Large Scale ◽  
Three Dimensional ◽  
Low Frequency ◽  
Bow Shock ◽  
Solar Wind Interaction ◽  
Ulf Wave ◽  
Upstream Condition ◽  
Upstream Solar Wind ◽  
The Imf

ABSTRACT We study the solar wind interaction with Mercury using a global three-dimensional hybrid model. In the analysed simulation run, we find a well-developed, dynamic Hermean ion foreshock ahead of the quasi-parallel bow shock under upstream solar wind and interplanetary magnetic field (IMF) conditions corresponding to the orbital perihelion of the planet. A portion of the incident solar wind ion flux is scattered back upstream near the quasi-parallel bow shock including both major solar wind ion species, protons and alphas. The scattered particles form the Hermean suprathermal foreshock ion population. A significant part of the suprathermal population is backstreaming with a velocity component towards the Sun in the near-foreshock at the planetocentric distance of few planetary radii in the plane of the IMF. The ion foreshock is associated with large-scale, oblique fast magnetosonic waves in the ultra-low-frequency (ULF) range convecting downstream with the solar wind. The ULF wave period is about 5 s in the analysed upstream condition case at Mercury, which corresponds to the 30-s foreshock waves at Earth when scaled by the IMF magnitude.

The solar wind interaction with Mars: results of three-dimensional three-species MHD studies

2001 ◽  
Vol 27 (11) ◽  
pp. 1837-1846 ◽  
Author(s):  
Y. Liu ◽  
A.F. Nagy ◽  
T.I. Gombosi ◽  
D.L. DeZeeuw ◽  
K.G. Powell
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Solar Wind Interaction
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