Skip to main content
U.S. Department of Energy
Office of Scientific and Technical Information

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

Journal Article · · Journal of Geophysical Research; (United States)
; ;  [1];  [2]; ;  [3]
  1. Univ. of California, Los Angeles (USA)
  2. NASA Ames Research Center, Moffett Field, CA (USA)
  3. NASA Goddard Space Flight Center, Greenbelt, MD (USA)
The Venus box shock location has been measured at nearly 2,000 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 box shock cross section is circular and only weakly sensitive to changing EUV flux.
OSTI ID:
5257231
Journal Information:
Journal of Geophysical Research; (United States), Journal Name: Journal of Geophysical Research; (United States) Vol. 93:A6; ISSN 0148-0227; ISSN JGREA
Country of Publication:
United States
Language:
English

Similar Records

Factors controlling the location of the venus bow shock
Journal Article · Fri Jul 01 00:00:00 EDT 1983 · J. Geophys. Res.; (United States) · OSTI ID:5811746

Interplanetary magnetic field control of the Mars bow shock: Evidence for Venuslike interaction
Journal Article · Mon Jul 01 00:00:00 EDT 1991 · Journal of Geophysical Research; (United States) · OSTI ID:5224461

The Venus bow shock: Detached or attached
Journal Article · Mon Jan 31 23:00:00 EST 1977 · J. Geophys. Res.; (United States) · OSTI ID:7120367