Large-scale patterns of eolian sediment transport on Venus - Predictions for Magellan

Details Large-scale patterns of eolian sediment transport on Venus - Predictions for Magellan Large-scale patterns of eolian sediment transport on Venus - Predictions for Magellan

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990georl..17.1365s&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 17, Aug. 1990, p. 1365-1368.

Physics

10

Magellan Project (Nasa), Planetary Boundary Layer, Sediment Transport, Venus Atmosphere, Venus Surface, Wind Effects, Halos, Planetary Craters, Radar Imagery, Sands, Topography, Venera Satellites

Scientific paper

The atmosphere of Venus is likely to exert a major influence on the surface. Arecibo and Venera 15/16 observations of the population of impact craters with bright halos give direct evidence of surface modification, on the scale of centimeters, to smooth the surface on time scales of 50 - 250 my. Both chemical and mechanical modifications probably occur. Diurnal winds in the planetary boundary layer can transport particles. Using boundary layer theory, including the effects of topography, surface stresses and resulting transport and deposition of sand-size particles are calculated. Regional slopes are sites of largest surface stresses. Sand will be generally transported downhill, although there is a preferential net transport from east to west, in the same direction as the atmospheric superrotation. It is predicted here that streaks may be seen in the Magellan radar images which will indicate directions of net eolian transport on the surface of Venus.

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