The Solar System Evolution

The concepts on the spatially-periodic condensation in the solar system have been considered in the light of the general theory of the evolution of the solar system. It has been shown that as protodisks arise and compress, the role of hydromagnetic effects weakens. After the stage of spatially-periodic condensation and accretion, the concentration of gas in protodisks decreases and the role of hydromagnetic effects increases again. Specific features of the formation of planets near the Sun and satellites near the planets can be explained if these peculiarities of the evolution are taken into account. The corresponding role of the above processes has been evaluated numerically. The accretion of gas molecules both by jet streams arising after spatially-periodic condensation and by planet embryos has also been considered. Characteristic times of these processes have been estimated. The results obtained show that the general concept on the solar system evolution (Alfvén and Arrhenius, 1976) is in good agreement with the mechanism of spatially-periodic condensation, which takes place during the formation of primary rings of the solar and satellite systems (Gladyshev, 1977).