Abstract
The existing models of core and mantle formation in originally homogeneous planets are briefly analysed. The authors' model is constructed on the basis of the latest theory of accumulation of the Earth-group planets, employs geo-cosmochemical data, and is an extension and refinement of the Elasser-Birch scheme. A specific feature of the model is that the differentiation starts in the upper shell of an already formed planet, and propagates inward, being controlled by heating and by the Rayleigh-Taylor instability mechanism. Results of the calculations on the early stages of the evolution are given, taking into account both heat and mass transfers in the process of gravitational differentiation and thermal convection in a spherically symmetrical model.
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