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Wind interaction with falling ejecta - Origin of the parabolic features on VenusA 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.
Document ID
19920048483
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Vervack, Ronald J., Jr.
(NASA Headquarters Washington, DC United States)
Melosh, H. J.
(Arizona, University Tucson, United States)
Date Acquired
August 15, 2013
Publication Date
March 20, 1992
Publication Information
Publication: Geophysical Research Letters
Volume: 19
ISSN: 0094-8276
Subject Category
Lunar And Planetary Exploration
Accession Number
92A31107
Funding Number(s)
CONTRACT_GRANT: NAGW-428
Distribution Limits
Public
Copyright
Other

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