A numerical simulation of the geomagnetic sudden commencement: 2. Plasma processes in the main impulse

Details A numerical simulation of the geomagnetic sudden commencement: 2. Plasma processes in the main impulse A numerical simulation of the geomagnetic sudden commencement: 2. Plasma processes in the main impulse

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jgra..108.1417f&link_type=abstract

Journal of Geophysical Research, Volume 108, Issue A12, pp. SMP 3-1, CiteID 1417, DOI 10.1029/2002JA009763

Physics

14

Magnetospheric Physics: Magnetosphere/Ionosphere Interactions, Magnetospheric Physics: Numerical Modeling, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Magnetospheric Physics: Current Systems (2409), Magnetospheric Physics: Magnetospheric Configuration And Dynamics

Scientific paper

A geomagnetic sudden commencement (SC) is studied numerically based on a model of buffeting the magnetosphere by a solar wind density impulse. This paper treats two successive current systems in the main impulse (MI) phase. The two current systems have different current generating mechanisms. The first current generator appears behind the wavefront of a compressional disturbance launched by the impulse. The inertia current of the compressional mode is generated by free energy due to deceleration of plasma flows. A field-aligned current (FAC) is excited through mode conversion from the compressional wave in a VA gradient region. The magnetospheric flows and the ionospheric flows are not connected self-consistently to each other. The second generator is located in the tailward side of the cusp. It is the same as the generator of the region 1 current system. The current generated there is connected with the FAC with the region 1 sense via a diamagnetic current flowing around an isolated enhancement of pressure in the nightside equatorial magnetosphere. The pressure enhancement is induced through compression of the magnetospheric flank due to the solar wind impulse. In this period, plasma convection vortices appear both in the magnetosphere and in the ionosphere, which are correspondent to each other. This is a peculiar convection confined within the magnetosphere (the SC transient cell convection). This convection is driven though compression of the magnetospheric flank due to the solar wind impulse.

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