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Magnetosphere Environment from Solar System Planets/Moons to Exoplanets

  • Igor I. AlexeevEmail author
  • Maria S. Grygoryan
  • Elena S. Belenkaya
  • Vladimir V. Kalegaev
  • Maxim Khodachenko
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Part of the Astrophysics and Space Science Library book series (ASSL, volume 411)

Abstract

First we discuss the solar wind plasma interaction with the Solar System planets that have intrinsic magnetic fields : Mercury , Earth , Jupiter , and Saturn are discussed. As a result of such an interaction cavities, which are free from the solar wind plasma and occupied by the planetary magnetic field are created. These cavities are usually called magnetospheres are surrounded and bound by the magnetopause . The magnetopause preserved the planetary magnetic field penetration into the magnetosheath so that its impossible for the magnetosheath plasma flow to penetrate into the magnetosphere. The magnetosheath are placed between the bow shock and the magnetopause. The bow shock forms a boundary against the unshocked super Alvénic plasma flow. As demonstrated by the analysis of the Mercury, Earth, Jupiter, and Saturn magnetopauses, these surfaces can be well described by a paraboloid of revolution with different subsolar distances and flaring angles. Based on this fact an universal model of the planetary magnetosphere can be constructed. We chose the planets in the inner magnetospheres of which the magnetic field vectors have been measured by orbiting spacecraft magnetometers. The proposed models describe the basic physical processes that are responsible for the structure and dynamics of the planetary magnetospheres . Additionally to the inner planetary field the different magnetospheric sources of magnetic field are included in the model. Finally, we discuss how these magnetosphere models can be applied to exoplanets in a comparative way.

Keywords

Solar Wind Interplanetary Magnetic Field Stellar Wind Dipole Field Solar Wind Plasma 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Notes

Acknowledgements

The authors acknowledge the support by the International Space Science Institute (ISSI) in Bern, Switzerland and the ISSI team Characterizing stellar- and exoplanetary environments. The authors acknowledge the support by the Austrian Research Foundation FWF NFN project S116 ‘Pathways to Habitability: From Disks to Active Stars, Planets and Life’, and the related FWF NFN subproject, S116 606-N16 ‘Magnetospheric Electrodynamics of Exoplanets’. This work was also supported by the FWF project P21197-N16. Finally, the authors are thankful to the European FP7 project IMPEx (No. 262863).

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Copyright information

© Springer International Publishing Switzerland 2015

Authors and Affiliations

  • Igor I. Alexeev
    • 1
    Email author
  • Maria S. Grygoryan
    • 1
  • Elena S. Belenkaya
    • 1
  • Vladimir V. Kalegaev
    • 1
  • Maxim Khodachenko
    • 1
    • 2
  1. 1.Scobeltsyn Institute of Nuclear PhysicsLomonosov Moscow State UniversityMoscowRussian Federation
  2. 2.Space Research InstituteAustrian Academy of SciencesGrazAustria

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