Numerical modelling of solar wind flow about nonaxisymmetric magnetospheres - Planets Jupiter and Saturn

Details Numerical modelling of solar wind flow about nonaxisymmetric magnetospheres - Planets Jupiter and Saturn Numerical modelling of solar wind flow about nonaxisymmetric magnetospheres - Planets Jupiter and Saturn

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997adspr..20..209f&link_type=abstract

Advances in Space Research, vol. 20, p. 209

Mathematics

1

Solar Wind, Jupiter Atmosphere, Planetary Magnetospheres, Saturn Atmosphere, Plasma Layers, Interplanetary Magnetic Fields, Magnetohydrodynamic Flow, Mathematical Models, Magnetosheath, Planetary Rotation

Scientific paper

The numerical integration of the dissipationless MHD equations under simplifying assumptions yields results on solar wind flow past Jupiter and Saturn, whose nonaxisymmetric, equatorially broadened magnetospheres are modeled as paraboloids with two different radii of curvature at the subsolar point. It is found that the thickness of the magnetosheath and the width and structure of the plasma depletion layer are strong functions of IMF orientation. These effects are more pronounced in the case of Jupiter than that of Saturn.

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