Abstract
The three-layer models of Mercury, Venus and Mars are constructed. Particularly, the model of Venus is investigated in detail. It is possible to construct the model of Venus with the same total iron content as in the Earth. High and low temperature models of Mercury and Mars are considered. The surface density of iron and silicates in the formation zones of the terrestrial planets is calculated and the results are compared with the surface density of the condensate in the formation zones of the giant planets. The principal shear stresses in the silicate mantles of the terrestrial planets are calculated using the data for nonequilibrium parts of the gravitational quadrupole moments. The viscosity distribution in the silicate mantles for all the planets are considered.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
