Boreskov

OP‐2Typical sizes of gravitational instabilities are equal in order of magnitude to the distancesbetween the planets. The masses of the rings of the local maximums of density comprisefractions of the masses of the corresponding planets.Fig. 1. Density iso‐contours at time=0.299.Fig. 2. Density iso‐contours at time=0.685.References[1]. V.S. Safronov. Accumulation of the planets. In: Origin of the solar system (Ed. G. Rivs), Publ.: Mir, Moscow,1976.[2]. A. V. Vityazev, G.V. Pechernikova, V.S. Safronov. Earth‐type planets: Origin and the early evolution. Publ.:Mir, Moscow, 1990.[3]. Ebert R., Habilitationschrift, Un. f. Frankfurt‐am‐Main, 1964.[4]. V.L. Polyachenko, A.M. Fridman. J. of Astronomy. V.49, No 1, p.157, 1972.[5]. A.V. Zabrodin, E.A. Zabrodina, M.S. Legkostupov, L.A. Pliner, K.V. Manukovskii. Some models of thedescription of proto‐planet solar disk at the initial stage of its evolution. Preprint KIAM RAS, No 70, 2006.[6]. A.V. Zabrodin, E.A. Zabrodina, M.S. Legkostupov, L.A. Pliner, K.V. Manukovskii. Some models of thedescription of proto‐planet solar disk at the initial stage of its evolution. In: Problems of origin andevolution of the biosphere (Ed. E.M. Galimov), Publ.: Librokom, Moscow, 2008, p. 297.[7]. S.K. Godunov , A.V. Zabrodin, and et al. Numerical solution of multidimensional problems of gas dynamics.Publ: Nauka, Moscow, 1976.33