Solar and interplanetary control of the location of the Venus bow shock

Details Solar and interplanetary control of the location of the Venus bow shock Solar and interplanetary control of the location of the Venus bow shock

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jgr....93.5461r&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 93, June 1, 1988, p. 5461-5469.

Physics

62

Bow Waves, Interplanetary Magnetic Fields, Shock Waves, Solar Planetary Interactions, Solar Wind, Venus Atmosphere, Dynamic Pressure, Magnetoacoustic Waves, Magnetohydrodynamic Flow, Plasma Pressure, Pressure Effects, Venus, Bow Shock, Position (Location), Magnetic Fields, Solar Wind, Flow, Distance, Pressure, Spacecraft Observations, Pvo Mission, Magnetosphere, Seasonal Variations, Wavelengths, Ultraviolet, Ionosphere

Scientific paper

The Venus bow shock location has been measured at nearly 2000 shock crossings, and its dependence on solar EUV, solar wind conditions, and the interplanetary magnetic field determined. The shock position at the terminator varies from about 2.14 Venus radii at solar minimum to 2.40 Venus radii at solar maximum. The location of the shock varies little with solar wind dynamic pressure but strongly with solar wind Mach number. The shock is farthest from Venus on the side of the planet in which newly created ions gyrate away from the ionosphere. When the interplanetary magnetic field is perpendicular to the flow, the cross section of the shock is quite elliptical. This effect appears to be due to the anisotropic propagation of the fast magnetosonic wave. When the interplanetary magnetic field is aligned with the flow, the bow shock cross section is circular and only weakly sensitive to changing EUV flux.

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