Dynamics of the tail in 3D PIC simulation of the magnetosphere during IMF rotation from north to south

Details Dynamics of the tail in 3D PIC simulation of the magnetosphere during IMF rotation from north to south Dynamics of the tail in 3D PIC simulation of the magnetosphere during IMF rotation from north to south

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm53a1437c&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM53A-1437

Physics

2723 Magnetic Reconnection (7526, 7835), 2744 Magnetotail, 2784 Solar Wind/Magnetosphere Interactions, 2790 Substorms

Scientific paper

Three dimensional PIC simulations are performed in order to analyse the dynamics of the magnetotail as the interplanetary magnetic field (IMF) rotates from northward to southward direction. This dynamics reveals to be quite different within meridan/equatorial planes over two successive phases of this rotation. First , as IMF rotates from North to Dawn-Dusk direction, the X-Point (magnetic reconnection) evidenced in the magnetotail (meridian plane) is moving earthward (from x=-35 Re to x=-17.5 ) distance at which it stabilizes. This motion is coupled with the formation of "Crosstail-S" patterns (within the plane perpendicular to the Sun-Earth mine) through the neutral sheet in the nearby magnetotail. Second, as IMF rotates from dawndusk to South, the minimum B field region is expanding within the equatorial plane and forms a ring . This two-steps dynamics is analyzed in strong association with the cross field magnetotail current Jy, in order to recover the signatures of substorms triggering.

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