Magnetospheric tails in the solar planetary system

Details Magnetospheric tails in the solar planetary system Magnetospheric tails in the solar planetary system

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986esasp.251..155m&link_type=abstract

In ESA Proceedings of the Joint Varenna-Abastumani International School and Workshop on Plasma Astrophysics p 155-161 (SEE N87-

Astronomy and Astrophysics

Astrophysics

1

Geomagnetic Tail, Jupiter (Planet), Planetary Magnetic Fields, Plasma-Electromagnetic Interaction, Astronomical Models, Magnetic Field Configurations, Plasma Density, Solar Wind

Scientific paper

Magnetospheric tails resulting from the interaction of a celestial body moving relative to the ambient magnetized plasma are discussed. A hydromagnetic model of a long planetary tail is presented. The tail is assumed to be a long structure in pressure equilibrium with the solar wind and with a partially open boundary. The model describes the basic properties (size, lobe, magnetic field, and plasma density) of the quiet distant terrestrial and jovian magnetotails as seen in the ISEE-3/and Voyager-1 data (at distances 200 Earth radii and 6000 Jupiter radii correspondingly behind the planets).

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