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The growth processes from protoplanetary dust to planetesimals are not fullyunderstood. Laboratory experiments and theoretical models have shown thatcollisions among the dust aggregates can lead to sticking, bouncing, andfragmentation. However, no systematic study on the collisional outcome ofprotoplanetary dust has been performed so far so that a physical model of thedust evolution in protoplanetary disks is still missing. We intend to map theparameter space for the collisional interaction of arbitrarily porous dustaggregates. This parameter space encompasses the dust-aggregate masses, theirporosities and the collision velocity. With such a complete mapping of thecollisional outcomes of protoplanetary dust aggregates, it will be possible tofollow the collisional evolution of dust in a protoplanetary disk environment.We use literature data, perform own laboratory experiments, and apply simplephysical models to get a complete picture of the collisional interaction ofprotoplanetary dust aggregates. In our study, we found four different types ofsticking, two types of bouncing, and three types of fragmentation as possibleoutcomes in collisions among protoplanetary dust aggregates. We distinguishbetween eight combinations of porosity and mass ratio. For each of these cases,we present a complete collision model for dust-aggregate masses between 10^-12and 10^2 g and collision velocities in the range 10^-4 to 10^4 cm/s forarbitrary porosities. This model comprises the collisional outcome, themass(es) of the resulting aggregate(s) and their porosities. We present thefirst complete collision model for protoplanetary dust. This collision modelcan be used for the determination of the dust-growth rate in protoplanetarydisks.

The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments