ИСТИНА

As analytical modeling shows (e. g., [1]), extensive internal water oceans could form due to 26Al decay and exist for a considerable time (~5 Myr or even more) at ~4 °C on large (R>100 km) rock-ice bodies in the early Solar system (ESS). After the early water differentiation, Edgeworth-Kuiper objects (EKOs) and pre-planetary bodies in the formation zones of giant planets were probably sources of icy and rock-organic matter after their breaking up at collisions. Intensive fluxes of the materials could considerably change surface mineralogy of asteroid parent bodies (APBs) in the main asteroid belt (MAB) shortly after their accretion. There is no doubt that a high surface density of matter in the formation zones of giant planets (especially, in Jupiter’s one) [2] led to runaway accretion of the planets themselves and smaller bodies. This ensured a short time of growth of large Jupiter zone bodies (JZBs) and enough 26Al in their interiors for complete melting water-ice except for the ~10-km crust and origin of a global water ocean [1]. Re-accretion of thick layers of JZBs' matter dispersed at collisions on the surfaces of several existed APBs could lead to formation of the largest C-type asteroids (as well as 1 Ceres and 2 Pallas). Considerable fragments of JZBs could become smaller members of the family or replenish close ones. Different groups of carbonaceous chondrites (CM2, CO, CV, etc.) would be formed in the same or other multiple processes of JZBs-APBs' and/or mutual APBs’ collisions depending on the number and intensity of the events. References: [1] Busarev et al. (2003), Earth, Moon & Plan-ets, 92, 345. [2] Safronov V. S. (1972) Evolution of the protoplanetary cloud and the formation of the Earth and the planets / TTF-667, Washington, 206 p.