Other
Scientific paper
Mar 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992georl..19..525v&link_type=abstract
Geophysical Research Letters (ISSN 0094-8276), vol. 19, March 20, 1992, p. 525-528.
Other
31
Ejecta, Magellan Spacecraft (Nasa), Planetary Craters, Venus Surface, Wind Effects, Astronomical Models, Impact Damage, Meteorite Craters
Scientific paper
A quantitative model in which the parabolic features are produced by the interaction of the zonal winds with material ejected ballistically from the impact crater is proposed. As the ejecta particles fall through the atmosphere, the winds transport them downwind from their entry point, smaller particles being transported a greater distance. Since the ejecta distribution is initially axially symmetric and smaller particles are thrown farther from the crater, the winds blow the particles on the upwind side back upon one another, leading to a pile-up of material. On the downwind side, the winds disperse the ejecta particles and no pile-up occurs. The resulting thickness distribution on the Venusian surface matches the observed parabolic features closely. The dual parabolic features associated with the crater Carson is also explained by this model.
Melosh Henry Jay
Vervack Ronald J. Jr.
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