A Protoplanetesimal Dust Collision Model Based on Experiments

Details A Protoplanetesimal Dust Collision Model Based on Experiments A Protoplanetesimal Dust Collision Model Based on Experiments

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf..412k&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.412

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Scientific paper

The formation of planets starts with the coagulation of small (sub-)millimeter sized dust particles in protoplanetary disks. Driven by their interaction with the surrounding gas, these particles collide at low velocities in the order of a few cm s-1 and stick at each other because of adhesive forces. This process leads to the formation of larger structures that are fractal at first. Due to the interaction with gas, the collision velocities rise, therefore the particles restructure and form compact but still very porous aggregates. Collisions among these particles do not necessarily lead to sticking. As these processes are not directly observable, our understanding of this first growth phase depends on theoretical models and experiments. In the last years, the physics of collisions between dust agglomerates of different sizes, porosities and materials has been studied in many laboratory experiments [2]. To reach the low collision velocities, which required for a realistic simulation of protoplanetary-disk conditions, most of the experiments were conducted under microgravity conditions, like in the drop tower in Bremen or on parabolic flights. The experiments have shown that the assumption that particles stick at each other for a wide velocity range and fragment if the velocity is sufficiently high enough, is not valid. In particular, we observed that collisions at intermediate velocities lead to bouncing.

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