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Migration of planetesimals from the feeding zone of the terrestrial planets,which was divided into seven regions depending on the distance to the Sun, wassimulated. The influence of gravity of all planets was taken into account. Insome cases, the embryos of the terrestrial planets rather than the planetsthemselves were considered; their masses were assumed to be 0.1 or 0.3 of thecurrent masses of the planets. The arrays of orbital elements of migratedplanetesimals were used to calculate the probabilities of their collisions withthe planets, the Moon, or their embryos. Based on our calculations, we drewconclusions on the process of accumulation of the terrestrial planets. Theembryos of the terrestrial planets, the masses of which did not exceed a tenthof the current planetary masses, accumulated planetesimals mainly from thevicinity of their orbits. When planetesimals fell onto the embryos of theterrestrial planets from the feeding zone of Jupiter and Saturn, these embryoshad not yet acquired the current masses of the planets, and the material ofthis zone (including water and volatiles) could be accumulated in the innerlayers of the terrestrial planets. The inner layers of each of the terrestrialplanets were mainly formed from the material located in the vicinity of theorbit of a certain planet. The outer layers of the Earth and Venus couldaccumulate the same material for these two planets from different parts of thefeeding zone of the terrestrial planets. The Earth and Venus could acquire morethan half of their masses in 5 Myr. A relatively rapid growth of the bulk ofthe Martian mass can be explained by the formation of Mars' embryo (the mass ofwhich is several times less than that of Mars) due to contraction of a rarefiedcondensation.

solar system research

Probabilities of collisions of planetesimals from different regions of  the feeding zone of the terrestrial planets with the forming planets and the  Moon