Gasdynamic modeling of the Venus magnetotail

Details Gasdynamic modeling of the Venus magnetotail Gasdynamic modeling of the Venus magnetotail

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jgr....96.5667m&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 96, April 1, 1991, p. 5667-5681. DOE-supported research.

Physics

15

Gas Dynamics, Planetary Magnetotails, Solar Planetary Interactions, Venus Atmosphere, Cold Plasmas, Oxygen Plasma, Solar Wind, Venus, Magnetosphere, Magnetotail, Models, Dynamics, Gases, Shape, Convection, Magnetic Field, Solar Wind, Comparisons, Parameters, Theoretical Studies, Plasma, Flow, Pressure, Oxygen, Density, Ions, Temperature, Pvo Mission, Spacecraft Observations, Pickup, Dayside, Ionosphere, Ionopause, Mass Loading, Opa Instrument, Particles, Distribution, Diagrams

Scientific paper

A gasdynamic, convected magnetic field model of the solar wind interaction with Venus is used to model the steady state Venus magnetotail. The flow obstacle surface is approximated as a tangential discontinuity. An initial obstacle shape is defined by balancing a hydrostatic equilibrium approximation for the internal plasma pressure with an external flow pressure approximation. These approximations produce a cylindrical obstacle in the distant tail. A refined obstacle shape that attempts to balance this internal pressure with the calculated external flow pressure tapers inward toward the tail axis downstream of the terminator. The bulk plasma flow and magnetic field properties compare well with experimental observations. The model predicts central magnetotail oxygen plasma number densities of about 0.2/cu cm and temperatures on the order of 10 to the 6th K flowing tailward at speeds as low as 200 m/s.

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