scholarly journals Three-dimensional full-kinetic simulation of the solar wind interaction with a vertical dipolar lunar magnetic anomaly

2016 ◽  
Vol 43 (9) ◽  
pp. 4136-4144 ◽  
Author(s):  
Jan Deca ◽  
Andrey Divin ◽  
Xu Wang ◽  
Bertrand Lembège ◽  
Stefano Markidis ◽  
...  
Keyword(s):  
Solar Wind ◽  
Magnetic Anomaly ◽  
Three Dimensional ◽  
Kinetic Simulation ◽  
Solar Wind Interaction

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 Solar wind interaction with the Reiner Gamma crustal magnetic anomaly: Connecting source magnetization to surface weathering

Icarus ◽  
2016 ◽  
Vol 266 ◽  
pp. 261-266 ◽  
Author(s):  
Andrew R. Poppe ◽  
Shahab Fatemi ◽  
Ian Garrick-Bethell ◽  
Doug Hemingway ◽  
Mats Holmström
Keyword(s):  
Solar Wind ◽  
Magnetic Anomaly ◽  
Solar Wind Interaction ◽  
Crustal Magnetic Anomaly

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

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
Sign in / Sign up

Export Citation Format

Share Document