Other
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p41a..01t&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #P41A-01
Other
[5475] Planetary Sciences: Solid Surface Planets / Tectonics, [5480] Planetary Sciences: Solid Surface Planets / Volcanism
Scientific paper
Loss of heat from planetary interiors is responsible for planetary volcanism and tectonics. On the earth plate tectonics plays the major role in this heat transport. Because Venus is similar in size to the earth it was reasonable to hypothesize that plate tectonics would occur on Venus. The Magellan mission showed conclusively that this is not the case. There are no ocean ridges on Venus but the coronae have been associated with subduction. The Magellan mission also showed that the surface on Venus is relatively young (0.5 to 1.0 Gyrs)and that the surface appears to be quiescent. How does heat escape from the interior of Venus? Plumes can transport some heat but instabilites of the surface thermal boundary layer are likely to dominate. This instability is expected to take the form of suduction and/or delamination. One hypothesis for Venusian heat loss is episodic subduction events followed by periods of relative quiescence. Many questions remain concerning the volcanic and tectonic evolution of Venus. Was there a primordial silicic crust? Do the volcanic plains cover this crust? Are the highlands made up of reworked silicic crust? Can new missions to Venus be proposed that would address these and other questions? Would an INSAR mission give fundamental new insights into the volcanism and tectonics on the planet.
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