Constraints on the thermal evolution of Venus inferred from Magellan data

Details Constraints on the thermal evolution of Venus inferred from Magellan data Constraints on the thermal evolution of Venus inferred from Magellan data

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992lpico.789....5a&link_type=abstract

In Lunar and Planetary Inst., Papers Presented to the International Colloquium on Venus p 5-6 (SEE N93-14288 04-91)

Computer Science

Convective Heat Transfer, Free Convection, Planetary Craters, Planetary Evolution, Planetary Geology, Planetary Temperature, Tectonics, Venus (Planet), Venus Surface, Volcanology, Cratering, Diffusion Coefficient, Lithosphere, Newtonian Fluids, Size Distribution, Spherical Shells, Statistical Distributions, Temperature Dependence, Thermal Diffusivity, Thermal Expansion, Three Dimensional Models, Time Dependence, Volcanoes

Scientific paper

The impact craters with diameters from 1.5 to 280 km compiled from Magellan observations indicate that the crater population on Venus has a completely spatially random distribution and the size/density distribution of craters with diameters greater than or equal to 35 km is consistent with a 'production' population with an age of 500 plus or minus 250 m.y. The similarity in size distribution from area to area indicates that the crater distribution is independent of crater size. Also, the forms of the modified craters are virtually identical to those of the pristine craters. These observations imply that Venus reset its cratering record by global resurfacing 500 m.y. ago, and resurfacing declined relatively fast. The fact that less than 40 percent of all craters have been modified and that the few volcanically embayed craters are located on localized tectonic regions indicate that only minor and localized volcanism and tectonism have occurred since the latest vigorous resurfacing event approximately 500 m.y. ago and the interior of Venus has been solid and possibly colder than Earth's. This is because the high-temperature lithosphere of Venus would facilitate upward ascending of mantle plumes and result in extensive volcanism if the venusian upper mantle were as hot as or hotter than Earth's. Therefore, the present surface morphology of Venus may provide useful constraints on the pattern of that vigorous convection, and possibly on the thermal state of the venusian mantle. We examine this possibility through numerical calculations of three-dimensional thermal convection models in a spherical shell with temperature- and pressure-dependent Newtonian viscosity, temperature-dependent thermal diffusivity, pressure-dependent thermal expansion coefficient, and time-dependent internal heat production rate solar magnitude.

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