Simulation of Pre-planetesimal Collisions with Smoothed Particle Hydrodynamics II

R. J. Geretshauser (), F. Meru, K. Schaal, R. Speith and W. Kley
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R. J. Geretshauser: Eberhard Karls Universität Tübingen, Institut für Astronomie und Astrophysik, Abteilung Computational Physics
F. Meru: Eberhard Karls Universität Tübingen, Institut für Astronomie und Astrophysik, Abteilung Computational Physics
K. Schaal: Eberhard Karls Universität Tübingen, Institut für Astronomie und Astrophysik, Abteilung Computational Physics
R. Speith: Eberhard Karls Universität Tübingen, Physikalisches Institut
W. Kley: Eberhard Karls Universität Tübingen, Institut für Astronomie und Astrophysik, Abteilung Computational Physics

A chapter in High Performance Computing in Science and Engineering ‘12, 2013, pp 51-67 from Springer

Abstract: Abstract In the frame of planet formation by coagulation the growth step from millimetre-sized highly porous dust aggregates to massive kilometre-sized planetesimals is not well constrained. In this regime of pre-planetesimals, collisional growth is endangered by disruptive collisions, disintegration by rotation as well as mutual rebound and compaction. Since laboratory studies of pre-planetesimal collisions are infeasible beyond centimetre-size, we perform numerical simulations. For this purpose, utilise the parallel smoothed particle hydrodynamics (SPH) code parasph. This program has been developed to simulate macroscopic highly porous dust aggregates consisting of protoplanetary material. We briefly introduce our porosity model and use it to perform simulations on the growth criteria of pre-planetesimals. With the aid of parameter studies we investigate fragmentation criteria in dust collisions depending on aggregate size and aggregate porosity. We extend a previous study on bouncing criteria of equally sized aggregates depending on their porosity and the presence of compacted shells of various porosities. Regarding the rotational stability of highly porous dust aggregates we theoretically derive fragmentation criteria for dust cylinders depending on angular velocity as well as porosity and perform suitable simulations.

Keywords: Filling Factor; Smooth Particle Hydrodynamic; Smooth Particle Hydrodynamic; Threshold Velocity; Protoplanetary Disc (search for similar items in EconPapers)
Date: 2013
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DOI: 10.1007/978-3-642-33374-3_6

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