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A highly favoured mechanism of planetesimal formation is collisional growth.Single dust grains, which follow gas flows in the protoplanetary disc, hit eachother, stick due to van der Waals forces and form fluffy aggregates up tocentimetre size. The mechanism of further growth is unclear since the outcomeof aggregate collisions in the relevant velocity and size regime cannot beinvestigated in the laboratory under protoplanetary disc conditions. Realisticstatistics of the result of dust aggregate collisions beyond decimetre size ismissing for a deeper understanding of planetary growth. Joining experimentaland numerical efforts we want to calibrate and validate a computer program thatis capable of a correct simulation of the macroscopic behaviour of highlyporous dust aggregates. After testing its numerical limitations thoroughly wewill check the program especially for a realistic reproduction of variousbenchmark experiments. We adopt the smooth particle hydrodynamics (SPH)numerical scheme with extensions for the simulation of solid bodies and amodified version of the Sirono porosity model. Experimentally measuredmacroscopic material properties of silica dust are implemented. We calibrateand test for the compressive strength relation and the bulk modulus. SPH hasalready proven to be a suitable tool to simulate collisions at rather highvelocities. In this work we demonstrate that its area of application can notonly be extended to low-velocity experiments and collisions. It can also beused to simulate the behaviour of highly porous objects in this velocity regimeto a very high accuracy.The result of the calibration process in this work isan SPH code that can be utilised to investigate the collisional outcome ofporous dust in the low-velocity regime.

Numerical Simulations of Highly Porous Dust Aggregates in the Low-Velocity Collision Regime