A thermomechanical model of the Earth's early evolution.

Details A thermomechanical model of the Earth's early evolution. A thermomechanical model of the Earth's early evolution.

Apr 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989izpse..24..846m&link_type=abstract

Izv. Acad. Sci. USSR, Phys. Solid Earth, Vol. 24, No. 10, p. 846 - 853

Physics

Earth: Protoplanets, Earth: Evolution

Scientific paper

Physical-mathematical models of planetary evolution are interpreted in terms of principles and equations of the mechanics of continuous media. Energy estimates are derived for the Earth. The boundary condition for the energy of growing protoplanets are specified. On the basis of a spherically symmetric one-component model, which includes equations of continuity, momentum (in the Stokes approximation), and energy and Poisson's equation for the gravity potential, the study examines the effects of compressibility and the characteristic stress formation and relaxation times (viscosity) upon the mechanical and thermal history of planets. For a low viscosity, analytic quasistationary solutions are obtained. In the general case, approximate solutions are constructed by the method of integral relations. The results of calculations depict the internal dynamics of a protoearth growing according to the Schmidt-Safronov hypothesis through attachment of variously sized particles from an alimentation zone.

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