Geological structure of the vicinity of Alpha Regio on Venus on the basis of data gathered by the Magellan spacecraft.

Details Geological structure of the vicinity of Alpha Regio on Venus on the basis of data gathered by the Magellan spacecraft. Geological structure of the vicinity of Alpha Regio on Venus on the basis of data gathered by the Magellan spacecraft.

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993sosyr..27....1i&link_type=abstract

Solar System Research, Vol. 27, No. 1, p. 1 - 13

Mathematics

Logic

Venus Surface: Geology, Venus Surface: Maps, Venus Surface: Structure

Scientific paper

Results of geological mapping of the area surrounding Alpha Regio on Venus on the basis of data gathered by the Magellan orbiters are presented. A stratigraphic approach is adopted, making it possible to order the divisions that have been identified in a scale in terms of their relative ages. The following divisions (from oldest to youngest) were established and correlated into a stratigraphic sequence of the mapland (five sheets of C1-MIDR format photographic charts were used): tesserae, hummocky plains; smooth plains; ridge belts; mottled plains; outer framework of corona; inner fill of corona; dark plains; individual lava flows; and impact craters. The geological history of the region is divided into two major stages, a tessera stage and a post-tessera stage. In the first stage (it has not been possible to establish the lower limit of this stage) the tesserae were formed. Tessera matter forms a basement which, in the course of the second stage, was covered with a stratified formation of lava plains. The population of the craters in the area appears to be a recent formation, superimposed on top of all the earlier divisions. Thus, the impact craters were built up following the termination of endogenic activity in this region. The age at which the region became stable, estimated from the density of the craters and on the basis of models of crater-forming flows, amounts to 0.5 - 1 Ga.

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