Dynamics of particle entries within the cusp boundary deformed during the IMF rotation from Northward to Southward: 3-D large-scale Particle-In-Cell simulation

Details Dynamics of particle entries within the cusp boundary deformed during the IMF rotation from Northward to Southward: 3-D large-scale Particle-In-Cell simulation Dynamics of particle entries within the cusp boundary deformed during the IMF rotation from Northward to Southward: 3-D large-scale Particle-In-Cell simulation

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm23a2035c&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM23A-2035

Physics

[2706] Magnetospheric Physics / Cusp, [2740] Magnetospheric Physics / Magnetospheric Configuration And Dynamics, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [7959] Space Weather / Models

Scientific paper

Large-scale global three-dimensional PIC simulations are performed with higher resolution (one grid size equal to 0.2 Earth radii) in order to analyze the dynamics of the cusp boundary formation and particle entry as the interplanetary magnetic field (IMF) rotates from northward to southward direction. As the IMF is northward, the ion and electron densities are strongly enhanced at the cusp boundaries, but electrons mainly accumulate along the outer edges of the cusp with a neat enhancement along the night-side edge, while ions fill in the inner part of the cusp. A "pile-up" of B field is observed along the outer edge of the cusp. Reconnection takes place at high elevation of the cusp and spreads along the magnetopause in the night side. The electron current is the strongest at the reconnection location. As the IMF turns dawn-dusk, new changes take place. The "pile-up" of B field is reinforced along the outer edge of the cusp, while the reconnection region shrinks and slightly moves to night side. The cusp itself fills-in with electrons everywhere while ions are mainly concentrated within the inner part of the cusp. However, particles penetrate (slightly) less deeply the cusp than with north IMF. When the IMF rotate form dawn-dusk to south, the "pile-up" of B field is weakened and shift toward North Pole. These results will be compared with experimental results issued from CLUSTER mission.

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