MAVEN observations of the Mars upper atmosphere, ionosphere, and solar wind interactions

2017 ◽  
Vol 122 (9) ◽  
pp. 9552-9553 ◽  
Author(s):  
Bruce M. Jakosky
Keyword(s):  
Solar Wind ◽  
Upper Atmosphere ◽  
Solar Wind Interactions

scholarly journals Space Weather, SuperDARN and the Tasmanian Tiger

1997 ◽  
Vol 50 (4) ◽  
pp. 773 ◽  
Author(s):  
Raymond A. Greenwald
Keyword(s):  
Solar Wind ◽  
Electric Fields ◽  
Space Weather ◽  
Interplanetary Space ◽  
Rapid Evolution ◽  
Upper Atmosphere ◽  
Global Network ◽  
Pressure Gradients ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

The plasma environment extending from the solar surface through interplanetary space to the outermost reaches of the Earth’s atmosphere and magnetic field is dynamic, often disturbed, and capable of harming humans and damaging manmade systems. Disturbances in this environment have been identified as space weather disturbances. At the present time there is growing interest in monitoring and predicting space weather disturbances. In this paper we present some of the difficulties involved in achieving this goal by comparing the processes that drive tropospheric-weather systems with those that drive space-weather systems in the upper atmosphere and ionosphere. The former are driven by pressure gradients which result from processes that heat and cool the atmosphere. The latter are driven by electric fields that result from interactions between the streams of ionised gases emerging from the Sun (solar wind) and the Earth’s magnetosphere. Although the dimensions of the Earth’s magnetosphere are vastly greater than those of tropospheric weather systems, the global space-weather response to changes in the solar wind is much more rapid than the response of tropospheric-weather systems to changing conditions. We shall demonstrate the rapid evolution of space-weather systems in the upper atmosphere through measurements with a global network of radars known as SuperDARN. We shall also describe how the SuperDARN network is evolving, including a newly funded Australian component known as the Tasman International Geospace Environmental Radar (TIGER).

A Global Survey of Geospace Electrons with eVlasiator: First Results

2021 ◽  
Author(s):  
Markku Alho ◽  
Markus Battarbee ◽  
Yann Pfau-Kempf ◽  
Urs Ganse ◽  
Lucile Turc ◽  
...  
Keyword(s):  
Solar Wind ◽  
Spatial Resolution ◽  
Kinetic Models ◽  
Electron Distribution ◽  
State Of The Art ◽  
Distribution Functions ◽  
Upper Atmosphere ◽  
Electron Precipitation ◽  
Gas Dynamic ◽  
First Results

<div> <p>Models of the geospace plasma environment have been proceeding towards more realistic descriptions of the solar wind—magnetosphere interaction, from gas-dynamic to MHD and hybrid ion-kinetic models such as the state-of-the-art Vlasiator model. Advances in computational capabilities have enabled global simulations of detailed physics, but the electron scale has so far been out of reach in a truly global setting. </p> </div><div> <p>In this work we present results from eVlasiator, an offshoot of the Vlasiator model, showing first results from a global 2D+3V kinetic electron geospace simulation. Despite truncation of some electron physics and use of ion-scale spatial resolution, we show that realistic electron distribution functions are obtainable within the magnetosphere and describe these in relation to MMS observations. Electron precipitation to the upper atmosphere from these velocity distributions is estimated.</p> </div>

scholarly journals MAVEN observations on a hemispheric asymmetry of precipitating ions toward the Martian upper atmosphere according to the upstream solar wind electric field

2017 ◽  
Vol 122 (1) ◽  
pp. 1083-1101 ◽  
Author(s):  
Takuya Hara ◽  
Janet G. Luhmann ◽  
François Leblanc ◽  
Shannon M. Curry ◽  
Kanako Seki ◽  
...  
Keyword(s):  
Solar Wind ◽  
Electric Field ◽  
Hemispheric Asymmetry ◽  
Upper Atmosphere ◽  
Upstream Solar Wind

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
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