THE INTRINSIC MAGNETIC FIELD AND SOLAR-WIND INTERACTION OF MARS

Mars ◽  
2018 ◽  
pp. 1090-1134 ◽  
Author(s):  
J. G. LUHMANN ◽  
C. T. RUSSELL ◽  
L. H. BRACE ◽  
O. L. VAISBERG
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Wind Interaction ◽  
Intrinsic Magnetic Field

Solar wind interaction with the Earth's magnetic field: 1. Magnetosheath

1973 ◽  
Vol 78 (19) ◽  
pp. 3714-3730 ◽  
Author(s):  
V. Formisano ◽  
G. Moreno ◽  
F. Palmiotto ◽  
P. C. Hedgecock
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Earth’S Magnetic Field ◽  
Solar Wind Interaction ◽  
Earth's Magnetic Field

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.

Solar Wind and Terrestrial Planets

2020 ◽  
Author(s):  
Edik Dubinin ◽  
Janet G. Luhmann ◽  
James A. Slavin
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Electric Fields ◽  
Interplanetary Space ◽  
Upper Atmosphere ◽  
Dipole Field ◽  
Terrestrial Planets ◽  
Solar Wind Interaction ◽  
Additional Energy ◽  
First Case

Knowledge about the solar wind interactions of Venus, Mars, and Mercury is rapidly expanding. While the Earth is also a terrestrial planet, it has been studied much more extensively and in far greater detail than its companions. As a result we direct the reader to specific references on that subject for obtaining an accurate comparative picture. Due to the strength of the Earth’s intrinsic dipole field, a relatively large volume is carved out in interplanetary space around the planet and its atmosphere. This “magnetosphere” is regarded as a shield from external effects, but in actuality much energy and momentum are channeled into it, especially at high latitudes, where the frequent interconnection between the Earth’s magnetic field and the interplanetary field allows some access by solar wind particles and electric fields to the upper atmosphere and ionosphere. Moreover, reconnection between oppositely directed magnetic fields occurs in Earth’s extended magnetotail—producing a host of other phenomena including injection of a ring current of energized internal plasma from the magnetotail into the inner magnetosphere—creating magnetic storms and enhancements in auroral activity and related ionospheric outflows. There are also permanent, though variable, trapped radiation belts that strengthen and decay with the rest of magnetospheric activity—depositing additional energy into the upper atmosphere over a wider latitude range. Virtually every aspect of the Earth’s solar wind interaction, highly tied to its strong intrinsic dipole field, has its own dedicated textbook chapters and review papers. Although Mercury, Venus, Earth, and Mars belong to the same class of rocky terrestrial planets, their interaction with solar wind is very different. Earth and Mercury have the intrinsic, mainly dipole magnetic field, which protects them from direct exposure by solar wind. In contrast, Venus and Mars have no such shield and solar wind directly impacts their atmospheres/ionospheres. In the first case, intrinsic magnetospheric cavities with a long tail are found. In the second case, magnetospheres are also formed but are generated by the electric currents induced in the conductive ionospheres. The interaction of solar wind with terrestrial planets also varies due to changes caused by different distances to the Sun and large variations in solar irradiance and solar wind parameters. Other important planetary differences like local strong crustal magnetization on Mars and almost total absence of the ionosphere on Mercury create new essential features to the interaction pattern. Solar wind might be also a feasible driver for planetary atmospheric losses of volatiles, which could historically affect the habitability of the terrestrial planets.

scholarly journals Solar wind interaction with the Earth's magnetosphere: the role of reconnection in the presence of a large scale sheared flow

2009 ◽  
Vol 16 (1) ◽  
pp. 1-10 ◽  
Author(s):  
F. Califano ◽  
M. Faganello ◽  
F. Pegoraro ◽  
F. Valentini
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Reconnection ◽  
Large Scale ◽  
Initial Conditions ◽  
Magnetic Layer ◽  
Magnetic Islands ◽  
Solar Wind Interaction ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

Abstract. The Earth's magnetosphere and solar wind environment is a laboratory of excellence for the study of the physics of collisionless magnetic reconnection. At low latitude magnetopause, magnetic reconnection develops as a secondary instability due to the stretching of magnetic field lines advected by large scale Kelvin-Helmholtz vortices. In particular, reconnection takes place in the sheared magnetic layer that forms between adjacent vortices during vortex pairing. The process generates magnetic islands with typical size of the order of the ion inertial length, much smaller than the MHD scale of the vortices and much larger than the electron inertial length. The process of reconnection and island formation sets up spontaneously, without any need for special boundary conditions or initial conditions, and independently of the initial in-plane magnetic field topology, whether homogeneous or sheared.

On the role of the magnetic field in the solar wind interaction with venus: Expectations versus observations

1981 ◽  
Vol 1 (1) ◽  
pp. 123-128 ◽  
Author(s):  
J.G. Luhmann ◽  
R.C. Elphic ◽  
C.T. Russell ◽  
L. Brace
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Wind Interaction ◽  
The Magnetic Field

Solar wind interaction with the Earth's magnetic field: 2. Magnetohydrodynamic bow shock

1973 ◽  
Vol 78 (19) ◽  
pp. 3731-3744 ◽  
Author(s):  
V. Formisano ◽  
P. C. Hedgecock ◽  
G. Moreno ◽  
F. Palmiotto ◽  
J. K. Chao
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Bow Shock ◽  
Earth’S Magnetic Field ◽  
Solar Wind Interaction ◽  
Earth's Magnetic Field

scholarly journals Open and partially closed models of the solar wind interaction with outer planet magnetospheres: the case of Saturn

2017 ◽  
Vol 35 (6) ◽  
pp. 1293-1308
Author(s):  
Elena S. Belenkaya ◽  
Stanley W. H. Cowley ◽  
Igor I. Alexeev ◽  
Vladimir V. Kalegaev ◽  
Ivan A. Pensionerov ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Neutral Line ◽  
Magnetized Plasma ◽  
Outer Planet ◽  
Solar Wind Interaction ◽  
Closed Model ◽  
Model Calculations ◽  
Open Model ◽  
The Imf

Abstract. A wide variety of interactions take place between the magnetized solar wind plasma outflow from the Sun and celestial bodies within the solar system. Magnetized planets form magnetospheres in the solar wind, with the planetary field creating an obstacle in the flow. The reconnection efficiency of the solar-wind-magnetized planet interaction depends on the conditions in the magnetized plasma flow passing the planet. When the reconnection efficiency is very low, the interplanetary magnetic field (IMF) does not penetrate the magnetosphere, a condition that has been widely discussed in the recent literature for the case of Saturn. In the present paper, we study this issue for Saturn using Cassini magnetometer data, images of Saturn's ultraviolet aurora obtained by the HST, and the paraboloid model of Saturn's magnetospheric magnetic field. Two models are considered: first, an open model in which the IMF penetrates the magnetosphere, and second, a partially closed model in which field lines from the ionosphere go to the distant tail and interact with the solar wind at its end. We conclude that the open model is preferable, which is more obvious for southward IMF. For northward IMF, the model calculations do not allow us to reach definite conclusions. However, analysis of the observations available in the literature provides evidence in favor of the open model in this case too. The difference in magnetospheric structure for these two IMF orientations is due to the fact that the reconnection topology and location depend on the relative orientation of the IMF vector and the planetary dipole magnetic moment. When these vectors are parallel, two-dimensional reconnection occurs at the low-latitude neutral line. When they are antiparallel, three-dimensional reconnection takes place in the cusp regions. Different magnetospheric topologies determine different mapping of the open-closed boundary in the ionosphere, which can be considered as a proxy for the poleward edge of the auroral oval.

Solar wind interaction with the Moon: Enhanced magnetic field fluctuations at low altitudes

1978 ◽  
Vol 5 (7) ◽  
pp. 592-594 ◽  
Author(s):  
H. Weiss ◽  
C. T. Russell ◽  
B. R. Lichtenstein ◽  
P. J. Coleman
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
The Moon ◽  
Solar Wind Interaction ◽  
Field Fluctuations
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