The magnetic barrier is a significant fraction of the magnetosheath region where magnetic forces react back on the plasma flow. We use a magnetohydrodynamic approach to calculate the solar wind flow around the magnetosphere. The use of so-called frozen-in coordinates, where the flow lines and the magnetic field are coordinate axes, is found to be most appropriate. Numerical solutions are presented for the problem of the flow around a blunt body. The results near the magnetopause are used as input parameters for a model of the reconnection of magnetic field lines based on shock-type structures.


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    Titel :

    The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause


    Beteiligte:
    Erkaev, N. V. (Autor:in) / Mezentsev, A. V. (Autor:in) / Biernat, H. K. (Autor:in) / Besser, B. P. (Autor:in) / Bachmaier, G. A. (Autor:in) / Semenov, V. S. (Autor:in) / Rijnbeek, R. P. (Autor:in) / Farrugia, C. J. (Autor:in)

    Erschienen in:

    Erscheinungsdatum :

    1994-07-01



    Medientyp :

    Sonstige


    Format :

    Keine Angabe


    Sprache :

    Englisch


    Schlagwörter :


    The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause

    Erkaev, N.V. / Mezentsev, A.V. / Biernat, H.K. et al. | Elsevier | 1994



    The Solar Wind Flow Along the Subsolar Line in the Magnetic Barrier and Reconnection at the Magnetopause

    Erkaev, N. V. / Mezentsev, A. V. / Biernat, H. K. et al. | British Library Conference Proceedings | 1994


    Why does the total pressure on the subsolar magnetopause differ from the solar wind dynamic pressure?

    Samsonov, A. A. / Němeček, Z. / Šafránková, J. et al. | Springer Verlag | 2013


    Why does the total pressure on the subsolar magnetopause differ from the solar wind dynamic pressure?

    Samsonov, A. A. / Němeček, Z. / Šafránková, J. et al. | Online Contents | 2013