A three dimensional gasdynamic model for solar wind flow past nonaxisymmetric magnetospheres - Application to Jupiter and Saturn

Details A three dimensional gasdynamic model for solar wind flow past nonaxisymmetric magnetospheres - Application to Jupiter and Saturn A three dimensional gasdynamic model for solar wind flow past nonaxisymmetric magnetospheres - Application to Jupiter and Saturn

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989jgr....9413353s&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 94, Oct. 1, 1989, p. 13353-13365.

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Gas Dynamics, Jupiter Atmosphere, Planetary Magnetospheres, Saturn Atmosphere, Solar Wind, Three Dimensional Models, Astronomical Models, Bow Waves, Planets, Jupiter, Saturn, Giant Planets, Gases, Dynamics, Solar Wind, Flow, Magnetosphere, Convection, Magnetic Fields, Models, Parameters, Symmetry, Magnetopause, Bow Shock, Diagrams, Numerical Methods, Shape, Calculations, Theoretical Studies, Comparisons

Scientific paper

The gasdynamic convected magnetic field model of Spreiter et al. (1966) and Spreiter and Stahara (1985) for predicting solar wind flow past a planetary magnetoionopause obstacle is extended to three dimensions and applied to Jupiter and Saturn, in which the effects of rapid spin, large size, and ring current phenomena are believed to result in broadening of their magnetospheres near the planetary equatorial plane. The computational procedures of the model are described, and the calculated results are presented for a number of magnetospheres of elliptic cross sections with values ranging from 1 to 2 for the ratio a/b between the major (equatorial) and minor (polar) axes. For Jupiter, the results indicate a broadening to a/b of about 1.754, a value consistent with previous estimates determined from independent calculations. For Saturn, a smaller broadening to a/b of about 1.25 is indicated.

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