MHD (Magnetohydrodynamic) simulation of a comet magnetosphere

Details MHD (Magnetohydrodynamic) simulation of a comet magnetosphere MHD (Magnetohydrodynamic) simulation of a comet magnetosphere

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984stin...8426546f&link_type=abstract

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Mathematics

Comet Tails, Cometary Magnetospheres, Comets, Magnetic Fields, Magnetohydrodynamics, Magnetospheres, Simulation, Solar Wind, Discontinuity, Interplanetary Magnetic Fields, Mathematical Models, Plasma Interactions, Rotation

Scientific paper

This paper presents results of a numerical magnetohydrodynamic simulation of the interaction of the solar wind with a comet. It states that for a steady solar wind and interplanetary magnetic field (IMF) the cometary plasma has a distinctive structure; a spheroidal head and a long ribbon-like tail. Rotational discontinuities in the IMF lead to changes in the tail structure. It is shown how these effects occur and describe ray-like structures as well as a tail disconnection event. The simulation results provide a simple explanation for a number of observable features in cometary plasma tails.

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