Page:Solar wind.djvu/9

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Rassbach, M. E., R. A. Wolf, and R. E, Daniell, Jr., 1974, "Convection in a Martian Magnetosphere," J. Geophys. Res., 79, p. 1125.
Spreiter, J. R., A. L. Summers, and A. Y. Alksne, 1966, "Hydromagnetic Flow Around the Magnetosphere," Planet. Space Sci., 14, p. 223.
Spreiter,J. R., A. Y. Alksne, and A. L. Summers, 1968, "External Aerodynamics of the Magnetosphere," Physics of the Magnetosphere, Caravillano, R. L., J. F. McClay, and H. R. Radoski, eds., Reidel, Dordrecht, Holland, p. 301.
Spreiter, J. R., A. L. Summers, and A. W. Rizzi, 1970, "Solar Wind Flow Past Nonmagnetic Planets-Venus and Mars," Planet. Space Sci., 18, p. 1281.

Cloutier/Galeev: The asymmetry of the ionopause which results from the difference in the drift of photoions across the ionopause in the cases of inward and outward interplanetary electric fields will be diminished by two effects:

  1. The collective interaction of photoions and solar-wind ions could prevent the photoions' acceleration up to solar-wind velocity and they will not experience a complete cycloidal trajectory.
  2. If the ionopause is diffuse, then the difference between the inward and outward electric field cases will be smaller.

Cloutier/Ness: I point out that the last figure in your talk (see figure 2(a) in Rassbach et al., 1974) is not a quantitative model but rather a schematic suggestion which does not bear a close relationship to the geometry of the observed conditions at Mars by the Mars-2, -3, and -5 spacecraft. That is, you indicate a very wide magnetosphere and tailward region which does not conform to the experimental observations of a much narrower tail region.

Cloutier/Vaisberg: Do you think azimuthal asymmetry of an obstacle necessarily leads to asymmetry of the bow shock, since an azimuthal component of the flow may develop due to the differences of an obstacle from a figure of rotation?

Cloutier: Yes, I think shock asymmetry will result from obstacle asymmetry.