The Abundance of Fine-Grained Impact Ejecta on Venus

Details The Abundance of Fine-Grained Impact Ejecta on Venus The Abundance of Fine-Grained Impact Ejecta on Venus

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..861m&link_type=abstract

Lunar and Planetary Science, volume 27, page 861

Physics

1

Ejecta: Impact, Fines, Processes: Surface, Venus

Scientific paper

The highly successful Magellan mission to Venus returned radar images that demonstrated the presence of aeolian deposits, wind streaks and dune fields, on the venusian surface. Although present, such deposits are not abundant, suggesting that fine "rained materials do not occur in large quantities on Venus. This is also consistent with the Venera lander images, which show broad areas of bare rock with only a thin mantle of coarse to fine clastic material. The source of even this small amount of loose material is unclear: Volcanic fire-fountaining may produce some fines, but how much of this activity is possible under Venus' elevated surface pressures is uncertain. Weathering in the terrestrial sense does not occur on Venus, so the release of resistant mineral grains by differential weathering is probably unimportant. In this abstract we estimate how much fine material is produced by impact craters, using data from craters with dark parabolic deposits. The final results show that the largest craters produce the largest volumes of fine material, and that the total volume thus produced is more than sufficient to account for all of the fine material observed. Thus, the dominant source of sand-sized fines on Venus may be ejecta from large impacts.

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