Other
Scientific paper
Mar 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28..755k&link_type=abstract
Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 755.
Other
Venus Surface, Ridges, Morphology, Planetary Surfaces, Planetary Gravitation
Scientific paper
Wrinkle ridges are known on all terrestrial bodies. They are thought to be compressional tectonic features resulted from folding followed by faulting or faulting followed by folding of a strong near-surface layer above weaker material. Watters (1991) measured frequency distributions of distances between wrinkle ridges for 15 areas on the Tharsis Plateau on Mars, where the ridges form quasi-periodical regional systems. He also measured widths and heights of 185 wrinkle-ridges-related features on the moon, Mars, and Mercury and subdivided them into ridges (with typical width/height ratio 10) and arches (width/height 70). On Venus, wrinkle ridges are more abundant than on other planets. They are common tectonic features on vast plains that occupy about 70 percent of Venus surface and play a key role in stratigraphy of Venus. In this paper, we report our measurements of Venusian wrinkle ridges morphometry and spacing of their net. We then compare our results with Watters' data for other planets.
Basilevsky Alexander T.
Kreslavsky Mikhail A.
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