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Context: Bouncing collisions of dust aggregates within the protoplanetary mayhave a significant impact on the growth process of planetesimals. Yet, theconditions that result in bouncing are not very well understood. Existingsimulations studying the bouncing behavior used aggregates with an artificial,very regular internal structure.  Aims: Here, we study the bouncing behavior of sub-mm dust aggregates that areconstructed applying different sample preparation methods. We analyze how theinternal structure of the aggregate alters the collisional outcome anddetermine the influence of aggregate size, porosity, collision velocity, andimpact parameter.  Methods: We use molecular dynamics simulations where the individualaggregates are treated as spheres that are made up of several hundred thousandindividual monomers. The simulations are run on GPUs.  Results: Statistical bulk properties and thus bouncing behavior of sub-mmdust aggregates depend heavily on the preparation method. In particular, thereis no unique relation between the average volume filling factor and thecoordination number of the aggregate. Realistic aggregates bounce only if theirvolume filling factor exceeds 0.5 and collision velocities are below 0.1 m/s.  Conclusions: For dust particles in the protoplanetary nebula we suggest thatthe bouncing barrier may not be such a strong handicap in the growth phase ofdust agglomerates, at least in the size range of 0.1 mm.

Bouncing Behavior of Microscopic Dust Aggregates