Differences between solar wind plasmoids and ideal magnetohydrodynamic filaments

Details Differences between solar wind plasmoids and ideal magnetohydrodynamic filaments Differences between solar wind plasmoids and ideal magnetohydrodynamic filaments

May 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981stin...8218110l&link_type=abstract

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Physics

Magnetohydrodynamic Flow, Magnetopause, Plasma-Electromagnetic Interaction, Plasmas (Physics), Solar Wind, Interplanetary Magnetic Fields, Lorentz Force, Magnetic Flux, Plasma Oscillations, Trapped Magnetic Fields

Scientific paper

The time dependent impulsive penetration model of solar wind plasma-magnetosphere interaction is elaborated on in order to emphasize its differences from ideal MHD models. The plasma-magnetic field entities differ from ideal MHD filaments. Their skin is not infinitely thin, but has a physical thickness determined by the gyromotion of the thermal ions and electrons. They are finite and their magnetic flux is interconnected with the interplanetary magnetic flux. When they penetrate into the magnetosphere their magnetic field lines become rooted in the ionosphere, i.e., in a medium with finite transverse conductivity. The external Lorentz force acting on their boundary surface depends on the orientation of their magnetic moment with respect to the external magnetic field. When their mechanical equilibrium is perturbed, hydromagnetic oscillations can be generated. The front side of all solar wind plasmoids which penetrate into the magnetosphere is considered to be the inner edge of the magnetospheric boundary layer, while the magnetopause is the surface where the magnetospheric plasma ceases to have a trapped pitch angle distribution.

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