Interaction of the solar wind with Mars and Venus over the solar cycle.

Details Interaction of the solar wind with Mars and Venus over the solar cycle. Interaction of the solar wind with Mars and Venus over the solar cycle.

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992cosre..30..322b&link_type=abstract

Cosmic Res., Vol. 30, No. 3, p. 322 - 341

Computer Science

Scientific paper

The results obtained on Phobos-2 and the results of earlier Mars missions (Mars-2, -3, and -5) are analyzed and compared. The properties of the boundaries observed in the region in which the solar wind interacts with Venus, Mars, and Comet Halley at solar minimum and solar maximum are also compared. There is an important similarity among these bodies of the solar system: a cometopause-like boundary forms near them. In the case of the planets, however, this boundary can form only during periods of high dynamic pressures of the solar wind or at the solar maximum. Mars is more comet-like than Venus. The boundary observed on Phobos-2, which was called a "magnetopause", is not a force-balance boundary. It has features similar to those of the cometopause at Comet Halley and in the upper boundary of the ionosphere of Venus during periods of high dynamic pressures of the solar wind. The obstacle in the solar wind near Mars at solar maximum may be either magnetospheric or ionospheric.

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