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- W196804586 abstract "At first, we develop the theory and show numerical simulations of solid-state convection of the Martian mantle. Available structural models of Mars have been studied in order to receive a basic model for our dynamical calculations of the Martian sphericalshell mantle. We newly derived thermal expansivity, activation volume and energy, Gruneisen parameter, melting temperatures, shear viscosity, and other parameters. Different sets of the distribution of the mentioned quantities result in different types of the convection planforms as a function of viscoplastic yield stress, Rayleigh number, Nusselt number and Urey number. Only in a few cases, we obtain an early Martian plate tectonics and the transfer to a one-plate planet. For comparison we present our results on the numerical simulation of the chemical differentiation of the Earth’s mantle. This differentiation induces the generation and growth of the continents and, as a complement, the formation and augmentation of the depleted MORB mantle. Here, we present for the first time a solution of this problem by an integrated theory in common with the problem of thermal convection in a 3-D compressible sphericalshell mantle. The whole coupled thermal and chemical evolution of mantle plus crust was calculated starting with the formation of the solid-state primordial silicate mantle. No restricting assumptions have been made regarding number, size and form of the continents. It was, however, implemented that moving oceanic plateaus touching a continent are to be accreted to this continent at the corresponding place. The model contains a mantle-viscosity profile with a usual asthenosphere beneath a lithosphere, a highly viscous transition zone and a second low-viscosity layer below the 660-km mineral phase boundary. The central part of the lower mantle is highly viscous. This explains the fact that there are, regarding the incompatible elements, chemically different mantle reservoirs in spite of perpetual stirring during more than 4.49 × 10 a. The highly viscous central part of the lower mantle also explains the relatively slow lateral movements of CMB-based plumes, slow in comparison with the lateral movements of the lithospheric plates. The temperatureand pressure-dependent viscosity of the model is complemented by a viscoplastic yield stress, σy . The paper includes a comprehensive variation of parameters, especially the variation of the viscosity-level parameter, rn, the yield stress, σy , and the temporal average of the Rayleigh number. In the rn-σy plot, a central area shows runs with realistic distributions and sizes of continents. This area is partly overlapping with the rn-σy areas of piecewise plate-like movements and of realistic values of the surface heat flow and Urey number." @default.
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- W196804586 date "2006-01-01" @default.
- W196804586 modified "2023-09-22" @default.
- W196804586 title "Preliminary dynamical models of thermal and chemical evolution of the mantles of Mars and Earth" @default.
- W196804586 hasPublicationYear "2006" @default.
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