Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p33a1423b&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #P33A-1423
Physics
5430 Interiors (8147)
Scientific paper
We have developed a numerical code to simulate the thermal convection in the mantle of the planets. The material of the mantle is approximated by the uncompressible newtonian fluid. The equations are solved by semi-spectral method. We have two versions of the code - 2D and 3D version. 3D version simulates thermal convection in a classical Boussinesq approximation in models with radially-dependent viscosity. 2D version uses extended Boussinesq approximation and general laterally variable viscosity. We use this code to study the internal dynamics of Venus. Important though indirect information about the structure of this planet provide the topography and the geoid. We use the results of Pauer et al., 2006, who analyze the Venusian geoid and topography and solve the inverse problem for viscosity. We use their best fitting viscosity models and carry out several simulations of mantle convection. We concentrate on the question how the geoid spectra computed in our convection models correspond with those of the observed data and how far is the Venusian mantle density structure from a simplified 2-D approximation used by Pauer et al. Further we study the effect of temperature-dependent viscosity and extended Boussinesq approximation.
Benesova N.
ČíŽKová Hana
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