Acceleration of ionospheric plasma clouds in the Venus ionosheath

Details Acceleration of ionospheric plasma clouds in the Venus ionosheath Acceleration of ionospheric plasma clouds in the Venus ionosheath

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000p%26ss...48..871p&link_type=abstract

Planetary and Space Science, Volume 48, Issue 9, p. 871-883.

Computer Science

3

Scientific paper

A discussion is presented to examine the acceleration and distribution of ionospheric plasma clouds around Venus. It is argued that magnetic forces may not be sufficient to accelerate those features and that their motion should also be influenced by the momentum of the solar wind around the flanks of the ionosheath. Plasma data obtained from selected Pioneer Venus Orbiter (PVO) passes show ionospheric clouds that have been displaced downstream from the planet, with a component directed away from the Venus plasma tail axis. The position and speed of these features suggests that they may not have been only accelerated by magnetic forces, but that most likely were also subject to effects produced by the kinetic energy of the solar wind. This suggestion derives from the observation of plasma tail rays with velocities comparable to the escape speed from the planet and also measurements of superalfvenic solar wind conditions around the flanks of the Venus ionosheath. While plasma clouds can be accelerated by magnetic forces near the subsolar region, where there is a strong accumulation of interplanetary magnetic field fluxes, the available experimental evidence shows that the Venus upper ionospheric plasma is accelerated mostly near the terminator, but not around the subsolar region. These views suggest that the ionospheric plasma clouds could be mostly accelerated around the flanks of the Venus ionosheath.

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