Boreskov

PL‐1first planetesimals (embryos of planet‐size bodies). The follow up evolutionary dynamics ofthe protoplanetary disc appears to involve the continuing processes of remaining dustclusters and planetesimals of different size collisions. Basically our dynamical models arefocused on the molecular dynamics approach and weighted Monte Carlo algorithms fornumerical evaluation of dust clusters formation including coagulation processes and solidbodies interaction under various physical‐chemical parameters and geometry. Peculiaritiesof gas‐dust clumps interaction with different mass ratio and collision velocities, as well asphysical mechanisms occurred in the contact zone of interacting solid bodies involvingenergy redistribution and some other non‐linear effects were investigated.The models developed allow us to distinguish between the more or less realisticmechanisms of planets grow from planetesimals incorporating chronology emerging fromradio nuclides isotopy. Some important questions remain open, however, in particular thoseabout stability maintenance of dust clusters and solid bodies within ring compression, timescale of the processes of interaction and phase transitions including, first of all, condensationand coagulation. These questions and prospects of further study are discussed in terms oftheir impact on the intriguing problem of life and biosphere origin.7