Computer Science
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008epsc.conf..203s&link_type=abstract
European Planetary Science Congress 2008, Proceedings of the conference held 21-25 September, 2008 in Münster, Germany. Online a
Computer Science
Scientific paper
ABSTRACT Mantle convection on Venus is likely to be in the stagnant lid regime of temperature-dependent viscosity convection in which only a thin bottom layer of the lithosphere participates in convection while the upper part of the lithosphere is stagnant because of its high viscosity. The longwavelength surface topography associated with mantle convection is due to the thermal thinning of the lithosphere (thermal isostasy) and mantle flow (dynamic topography). While in the constant viscosity or weakly variable viscosity convection the magnitudes of the two components are comparable, in the well-developed stagnant lid convection regime, the dynamic component is negligibly small. This suggests that the Venusian topography is largely controlled by isostasy.
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