3D MHD Description and Animation of the Process of Collision of a Solar Wind Shock with the Earth’s Bow Shock
At present, several groups of spacecraft in the vicinity of the Earth’s bow shock S b , magnetosheath, and outer magnetosphere and spacecraft located in the free solar wind stream near the Lagrange point L 1 are measuring the magnetosphere and solar wind parameters and the interplanetary magnetic field (IMF). The data obtained on the Earth are analyzed to forecast the cosmic weather, in particular, to identify sharp changes in the solar wind associated with shock waves [1, 2]. For interpreting adequately spacecraft’s measurements it is necessary to have exact solutions of the problem of interaction between a solar wind discontinuity and the bow shock in which the wave flow pattern is known as a function of coordinates of a point on S b .
KeywordsSolar Wind Interplanetary Magnetic Field Rarefaction Wave Solar Wind Parameter Tangential Discontinuity
Unable to display preview. Download preview PDF.
- 1.Přech, L., Němeček, Z., Šafránková, J.: Geophys. Res. Lett. 35, L17S02 (2008)Google Scholar
- 2.Keika, K., Nakamura, R., Baumjohann, W., et al.: J. Geophys. Res. 114, A00C24 (2009)Google Scholar
- 5.Pushkar, E.A., Barmin, A.A., Grib, S.A.: Geomegnetizm i Aeronomiya 31(3), 522–525 (1991)Google Scholar
- 7.Grib, S.A., Pushkar, E.A.: Geomegnetizm i Aeronomiya 46(4), 442–448 (2006)Google Scholar