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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 21, issue 5
Ann. Geophys., 21, 1083–1093, 2003
https://doi.org/10.5194/angeo-21-1083-2003
© Author(s) 2003. This work is distributed under
the Creative Commons Attribution 3.0 License.
Ann. Geophys., 21, 1083–1093, 2003
https://doi.org/10.5194/angeo-21-1083-2003
© Author(s) 2003. This work is distributed under
the Creative Commons Attribution 3.0 License.

  31 May 2003

31 May 2003

Penetration of magnetosonic waves into the magnetosphere: influence of a transition layer

A. S. Leonovich3,1, V. V. Mishin3,1, and J. B. Cao2,3 A. S. Leonovich et al.
  • 1Institute of Solar-Terrestrial Physics (ISTP), Russian Academy of Science, Siberian Branch, Irkutsk 33, P.O.Box 4026, 664033, Russia
  • 2Center for Space Science and Applied Research, Chinese Academy of Science, China
  • 3Russian-Chinese Joint Research Center on Space Weather, China

Abstract. We have constructed a theory for the penetration of magnetosonic waves from the solar wind into the magnetosphere through a transition layer in a plane-stratified model for the medium. In this model the boundary layer is treated as a region, inside of which the parameters of the medium vary from values characteristic for the magnetosphere, to values typical of the solar wind. It is shown that if such a layer has sufficiently sharp boundaries, then magnetosonic eigen-oscillations can be excited inside of it. The boundaries of such a layer are partially permeable for magnetosonic waves. Therefore, if the eigen-oscillations are not sustained by an external source, they will be attenuated, because some of the energy is carried away by the oscillations that penetrate the solar wind and the magnetosphere. It is shown that about 40% of the energy flux of the waves incident on the transition layer in the magnetotail region penetrate to the magnetosphere’s interior. This energy flux suffices to sustain the stationary convection of magnetospheric plasma. The total energy input to the magnetosphere during a time interval of the order of the substorm growth phase time is comparable with the energetics of an average substorm.

Key words. Magnetospheric physics (MHD waves and instabilities; solar wind–magnetosphere interactions) – Space plasma physics (kinetic and MHD theory)

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