The solar wind interaction with Mars revisited

Abstract

No consensus has yet been reached on the nature of the solar wind interaction with Mars, especially with respect to the existence of a small, intrinsic field magnetosphere at Mars, as opposed to a Venus-like ionospheric interaction. An attempt is made to resolve this question through an improved determination of effective obstacle altitude and shape having as its basis the Spreiter and Stahara (1980) catalog of gasdynamic flow solutions. It is also shown that the Martian ionosphere cannot support a Venus-like ionopause at the obstacle altitudes inferred through bow wave observation modelling, even when maximal induced ionospheric magnetic fields and solar maximum EUV levels are assumed. Finally, a search of Mars and Mariner radio occultation measurements has produced no evidence for the existence of an ionopause. It is concluded that Mars probably possesses a small, intrinsic field magnetosphere.