Abstract
Our investigations of the migration of bodies in the Solar system and the formation of planets were based mainly on the results of computer simulation of the evolution of disks that originally consisted of hundreds of gravitating bodies moving around the Sun (Ipatov 1987, 1993a). The mutual gravitational influence of bodies was taken into account by the Tisserand spheres method, that is two two-bodies problems were considered. Ipatov (1988a) also made analytical studies of the dependence of the time of disk evolution as a function of the number of bodies constituting the disk. For choosing the pairs of encounting (up to the radius of the Tisserand sphere) bodies, Ipatov (1993b) used the probability and deterministic methods. For the probability method, the pairs of encounting bodies were chosen proportionally to the probabilities of their encounters. For the deterministic method, the time to an isolated (from other bodies) encounter of the pair of encounting bodies was minimum. To our opinion, the deterministic method is more physical. Orbits and masses of formed planets, and times to collisions of separate bodies with planets are almost identical for both methods. However, the time of the evolution of disks, consisting of a large number of bodies, and so the time of the formation of the main part of planets’ masses obtained by using the deterministic method are ten times less than those obtained by using the probability one. In particular, the time to form 80 % of mass of the Earth did not exceed 10 Myr.
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© 1995 Springer Science+Business Media Dordrecht
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Ipatov, S.I. (1995). Migration of Bodies in the Accumulation of Planets. In: Chahine, M.T., A’Hearn, M.F., Rahe, J., Solomon, P., Nickle, N.L. (eds) Comparative Planetology with an Earth Perspective. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-1092-3_20
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DOI: https://doi.org/10.1007/978-94-017-1092-3_20
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