Diversity of planetary systems from evolution of solids in protoplanetary disks

We have developed and applied a model designed to track simultaneously the evolution of gas and solids in protoplanetary disks from an early stage, wh en all solids are in the dust form, to the stage when most solids are in th e form of a planetesimal swarm. The model is computationally efficient and allows for a global, comprehensive approach to the evolution of solid parti cles due to gas-solid coupling, coagulation, sedimentation, and evaporation /condensation. The co-evolution of gas and solids is calculated for 10(7) y r for several evolution regimes and starting from a comprehensive domain of initial conditions. The output of a single evolutionary run is a spatial d istribution of mass locked in a planetesimal swarm. Because swarm's mass di stribution is related to the architecture of a nascent planetary system, di versity of swarms is taken as a proxy for a diversity of planetary systems. We have found that disks with low values of specific angular momentum are bled out of solids and do not form planetary systems. Disks with high and i ntermediate values of specific angular momentum form diverse planetary syst ems. Solar-like planetary systems form from disks with initial masses less than or equal to0.02 M-circle dot and angular momenta less than or equal to 3x10(52) g cm(2) s(-1). Planets more massive than Jupiter can form at loca tions as close as 1 AU from the central star according to our model.