A 3-D computational model for solar wind/magnetosphere interactions - Prediction of polar flattening of Jupiter and Saturn magnetospheres

Details A 3-D computational model for solar wind/magnetosphere interactions - Prediction of polar flattening of Jupiter and Saturn magnetospheres A 3-D computational model for solar wind/magnetosphere interactions - Prediction of polar flattening of Jupiter and Saturn magnetospheres

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987aiaa.confq....s&link_type=abstract

AIAA, Fluid Dynamics, Plasma Dynamics, and Lasers Conference, 19th, Honolulu, HI, June 8-10, 1987. 11 p.

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Computation

Computational Astrophysics, Jupiter Atmosphere, Planetary Magnetospheres, Saturn Atmosphere, Solar Planetary Interactions, Solar Wind, Three Dimensional Models, Bow Waves, Conservation Laws, Magnetic Field Configurations, Magnetohydrodynamics, Magnetosheath

Scientific paper

The development of a computational model for determining the solution of the gasdynamic portion of the gasdynamic convected magnetic field model for solar wind flow past three-dimensional magnetoionopauses of nonaxisymmetric shape is described. Results are presented for the shape of the bow wave and the flow properties in magnetosheaths of polar flattened magnetopauses representative of Jupiter and Saturn. Through a parametric study in which the amount of polar flattening is varied, a quantitative determination is obtained of the degree of flattening at both Jupiter and Saturn. These new three-dimensional results are shown to be in good agreement with observations, and account for most of the differences between the observations and the axisymmetric model results.

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