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Coagulation of dust aggregates plays an important role in the formation ofplanets and is of key importance to the evolution of protoplanetary disks(PPDs). Characteristics of dust, such as the diversity of particle size,porosity, charge, and the manner in which dust couples to turbulent gas, affectthe collision outcome and the rate of dust growth. Here we present a numericalmodel of the evolution of the dust population within a PPD which incorporatesall of these effects. The probability that any two particles collide depends onthe particle charge, cross-sectional area and their relative velocity. Theactual collision outcome is determined by a detailed collision model whichtakes into account the aggregate morphology, trajectory, orientation, andelectrostatic forces acting between charged grains. The data obtained in thisresearch reveal the characteristics of dust populations in differentenvironments at the end of the hit-and-stick growth, which establishes thefoundation for the onset of the next growth stage where bouncing, mass transferand fragmentation become important. For a given level of turbulence, neutraland weakly charged particles collide more frequently and grow faster thanhighly charged particles. However, highly charged particles grow to a largersize before reaching the bouncing barrier, and exhibit a "Runaway" growth, inwhich a few large particles grow quickly by accreting smaller particles whilethe rest of the population grows very slowly. In general, highly chargedaggregates have a more compact structure and are comprised of larger monomersthan neutral/weakly charged aggregates. The differences in the particlestructure/composition not only affect the threshold velocities for bouncing andfragmentation, but also change the scattering and absorption opacity of dust,influencing the appearance of PPDs.

Detailed Model of the Growth of Fluffy Dust Aggregates in a Protoplanetary Disk: Effects of Nebular Conditions