Numerical studies on magnetotail formation and driven reconnection

Details Numerical studies on magnetotail formation and driven reconnection Numerical studies on magnetotail formation and driven reconnection

May 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jgr....90.4035m&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 90, May 1, 1985, p. 4035-4045.

Statistics

Computation

25

Computational Astrophysics, Earth Magnetosphere, Geomagnetic Tail, Solar Wind, Space Plasmas, Boundary Layer Plasmas, Electrical Resistivity, Flux (Rate), Magnetic Field Configurations, Magnetohydrodynamics, Plasma Interactions, Shock Waves, Solar Flares, Steady State

Scientific paper

The present investigation is concerned with the development of an MHD simulation model, taking into account the study of a two-dimensional formation of magnetotail starting from a dipole magnetic field. It is observed that a two-dimensional tail-like structure develops associated with the plasma flow originating from the solar wind. The obtained results, such as plasma sheet thinning, strong plasma jetting, and the plasmoid motion, appear to be in good agreement with satellite observations. It is believed that the magnetospheric substorm can be caused by reconnection driven by the solar wind plasmas entering the magnetosphere, presumably as a result of dayside reconnection.

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