A three-dimensional diffusion/convection model of the large scale magnetic field in the Venus ionosphere

Details A three-dimensional diffusion/convection model of the large scale magnetic field in the Venus ionosphere A three-dimensional diffusion/convection model of the large scale magnetic field in the Venus ionosphere

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jgr....93.5909l&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 93, June 1, 1988, p. 5909-5914.

Physics

9

Atmospheric Diffusion, Atmospheric Models, Planetary Ionospheres, Planetary Magnetic Fields, Three Dimensional Models, Venus Atmosphere, Atmospheric Physics, Convection, Dynamo Theory, Magnetohydrodynamic Flow, Solar Wind, Venus, Diffusion, Convection, Models, Magnetic Fields, Ionosphere, Solar Wind, Interaction, Magnetosheath, Parameters, Diagrams, Spacecraft Observations, Pvo Mission, Calculations

Scientific paper

A three-dimensinal diffusion/convection model of the dayside Venus ionosphere magnetic field was developed on the basis of previously published one-dimensional diffusion/convection models, and assuming that the field and flow at the upper boundary (in the magnetic barrier) as well as the ionospheric plasma velocity are known. The results indicate that the low-altitude magnetosheath field draping may be distorted by the interaction with the ionosphere in such a manner that there is an apparent 'focusing' of the field toward the subsolar point, caused by the shear in the horizontal velocity between the magnetosheath and ionospheric flows. A comparison of published magnetic-field observations with the present results indicates that the simple nesting of external and internal velocity fields may be a good approximation to global plasma flows near Venus under normal conditions.

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