Nature of solar wind interaction with Venus

Details Nature of solar wind interaction with Venus Nature of solar wind interaction with Venus

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978kosis..16..746r&link_type=abstract

(International Association of Geomagnetism and Aeronomy, Scientific Assembly, 3rd, Seattle, Wash., Aug. 22-Sept. 3, 1977.) Kosmi

Physics

3

Ion Motion, Plasma Interactions, Solar Planetary Interactions, Solar Wind, Venus Atmosphere, Electrostatic Probes, Gas Dynamics, Magnetospheric Instability, Planetary Magnetic Fields, Planetary Magnetospheres, Plasmapause, Shock Fronts, Shock Wave Profiles, Venera Satellites

Scientific paper

Ion flux data obtained by Venera 9 and 10 are analyzed. It is shown that the solar wind flux past Venus can be satisfactorily described by a gasdynamic model, in the first approximation. Evidence is presented for the asymmetry of the shock wave at the planet and the association between this asymmetry with the anisotropy of the solar wind. The boundary of the Venusian magnetoplasma tail (ionopause) at the dark side has a length of five Venusian radii; the high-energy particle bursts near this boundary are associated with the turbulent zone at the tail boundary. The boundary layer at the upperside of the tail is due to viscosity effects arising in the interaction of the solar wind with the induced Venusian magnetosphere.

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