Mathematics – Logic
Scientific paper
Mar 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000jgr...105.6983d&link_type=abstract
Journal of Geophysical Research, Volume 105, Issue E3, p. 6983-6996
Mathematics
Logic
17
Planetology: Solid Surface Planets: Origin And Evolution, Planetology: Solid Surface Planets: Tectonics, Planetology: Solid Surface Planets: Volcanism, Planetology: Solar System Objects: Venus
Scientific paper
Geologic mapping of southern Rusalka Planitia, Venus, reveals interactions of volcanism, tectonism, and topography. We recognize three regional plains units (prR1, prR2, and prR3) based on crosscutting structural relations, embayment patterns, radar brightness, and surface roughness data. Delineation of secondary (tectonic) structures allows us to constrain the relative temporal relations between the three material units. Unit prR1, a radar dark smooth unit exposed in local topographic highs, hosts NE trending extension fractures. Low-viscosity lava flows of prR2, the most areally extensive unit, fill local topographic lows and the NE trending fractures. A shield-sourced lava unit, prR3, overlies prR2 on the basis of embayment relations and radar brightness. NW trending wrinkle ridges deform all three plains units and record regional contraction. Locally, flood lava flows that fill NE trending fractures are structurally inverted to form short, stepped NE trending wrinkle ridges. Map patterns indicate that prR2 comprises a thin layer (<50 m thick), much thinner than previous estimates of 1-3 km. Therefore previously proposed estimates of plains flood lava flow volumes and effusion rates are much too high. The local geologic history of southern Rusalka Planitia is inconsistent with global stratigraphy models. Our study supports the view of plains evolution occurring through discrete volcanic processes working at local and regional (but not global) scales.
Deshon Heather R.
Hansen Vicki L.
Young Duncan A.
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