The magnetosphere of Uranus - Plasma sources, convection, and field configuration

Details The magnetosphere of Uranus - Plasma sources, convection, and field configuration The magnetosphere of Uranus - Plasma sources, convection, and field configuration

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...266..390v&link_type=abstract

Astrophysical Journal, Part 1, vol. 266, Mar. 1, 1983, p. 390-401.

Physics

Plasma Physics

24

Convective Flow, Magnetic Field Configurations, Planetary Magnetospheres, Plasma Currents, Solar Wind, Thermal Plasmas, Uranus Atmosphere, Atmospheric Models, Interplanetary Magnetic Fields, Magnetohydrodynamics, Plasma Physics, Plasma Pressure, Plasma-Electromagnetic Interaction, Voyager 2 Spacecraft, Uranus, Magnetosphere, Plasma, Sources, Convection, Shape, Structure, Magnetic Properties, Dipole Moment, Hypotheses, Geometry, Current Sheet, Pressure, Magnetotail, Magnetopause, Models, Solar Wind, Calculat

Scientific paper

It is suggested by qualitative considerations based on analogy with earth, Jupiter, and Saturn that the magnetosphere of Uranus may lack a plasma source able to produce significant internal currents, internal convection, and associated effects. A class of approximately self-consistent quantitative magnetohydrostatic equilibrium configurations for the case of a pole-on magnetosphere with variable plasma parameters is presently constructed in order to test this hypothesis by means of forthcoming Voyager measurements. The configurations that can be computed for the geometries of the magnetic field and of the tail current sheet, for a given distribution of plasma pressure, have a single, funnel-shaped polar cusp pointing into the solar wind and a cylindrical tail plasma sheet whose currents close within the tail, rather than on the tail magnetopause. Interconnection of interplanetary and magnetospheric fields yields a highly asymmetric tail-field configuration.

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