Solar wind interaction with the Martian upper atmosphere: Crustal field orientation, solar cycle, and seasonal variations

2015 ◽  
Vol 120 (9) ◽  
pp. 7857-7872 ◽  
Author(s):  
Chuanfei Dong ◽  
Stephen W. Bougher ◽  
Yingjuan Ma ◽  
Gabor Toth ◽  
Yuni Lee ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Seasonal Variations ◽  
Upper Atmosphere ◽  
Solar Wind Interaction ◽  
Field Orientation ◽  
Crustal Field

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.

DYNAMO: a Mars upper atmosphere package for investigating solar wind interaction and escape processes, and mapping Martian fields

2004 ◽  
Vol 33 (12) ◽  
pp. 2228-2235 ◽  
Author(s):  
E. Chassefière ◽  
A. Nagy ◽  
M. Mandea ◽  
F. Primdahl ◽  
H. Rème ◽  
...  
Keyword(s):  
Solar Wind ◽  
Upper Atmosphere ◽  
Solar Wind Interaction

scholarly journals Multifluid MHD study of the solar wind interaction with Mars' upper atmosphere during the 2015 March 8th ICME event

2015 ◽  
Vol 42 (21) ◽  
pp. 9103-9112 ◽  
Author(s):  
Chuanfei Dong ◽  
Yingjuan Ma ◽  
Stephen W. Bougher ◽  
Gabor Toth ◽  
Andrew F. Nagy ◽  
...  
Keyword(s):  
Solar Wind ◽  
Upper Atmosphere ◽  
Solar Wind Interaction

scholarly journals Solar Wind Interaction With the Martian Upper Atmosphere: Roles of the Cold Thermosphere and Hot Oxygen Corona

2018 ◽  
Vol 123 (8) ◽  
pp. 6639-6654 ◽  
Author(s):  
Chuanfei Dong ◽  
Stephen W. Bougher ◽  
Yingjuan Ma ◽  
Yuni Lee ◽  
Gabor Toth ◽  
...  
Keyword(s):  
Solar Wind ◽  
Upper Atmosphere ◽  
Solar Wind Interaction ◽  
Hot Oxygen

scholarly journals Effects of a dipole-like crustal field on solar wind interaction with Mars

2020 ◽  
Vol 4 (1) ◽  
pp. 1-9
Author(s):  
ShiBang Li ◽  
◽  
HaoYu Lu ◽  
Jun Cui ◽  
YiQun Yu ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Interaction ◽  
Crustal Field

scholarly journals Solar wind interaction with Mars upper atmosphere: Results from the one-way coupling between the multifluid MHD model and the MTGCM model

2014 ◽  
Vol 41 (8) ◽  
pp. 2708-2715 ◽  
Author(s):  
Chuanfei Dong ◽  
Stephen W. Bougher ◽  
Yingjuan Ma ◽  
Gabor Toth ◽  
Andrew F. Nagy ◽  
...  
Keyword(s):  
Solar Wind ◽  
Upper Atmosphere ◽  
Solar Wind Interaction ◽  
Mhd Model ◽  
The One

The solar wind interaction with Venus through the eyes of the Pioneer Venus Orbiter

2006 ◽  
Vol 54 (13-14) ◽  
pp. 1482-1495 ◽  
Author(s):  
C.T. Russell ◽  
J.G. Luhmann ◽  
R.J. Strangeway
Keyword(s):  
Solar Wind ◽  
Solar Wind Interaction
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