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High-resolution simulations of planetesimal formation in turbulent protoplanetary discs
Johansen, Anders; Klahr, Hubert; Henning, Thomas
AA(Lund Observatory, Lund University, Box 43, 221 00 Lund, Sweden ), AB(Max-Planck-Institut für Astronomie Königstuhl 17, 69117 Heidelberg, Germany), AC(Max-Planck-Institut für Astronomie Königstuhl 17, 69117 Heidelberg, Germany)
The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution, Proceedings of the International Astronomical Union, IAU Symposium, Volume 276, p. 89-94
Publication Date:
accretion, accretion disks, MHD, turbulence, planetary systems: formation, planetary systems: protoplanetary disks
Abstract Copyright:
(c) 2011: Copyright © International Astronomical Union 2011
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We present high resolution computer simulations of dust dynamics and planetesimal formation in turbulence triggered by the magnetorotational instability. Particles representing approximately meter-sized boulders clump in large scale overpressure regions in the simulation box. These overdensities readily contract due to the combined gravity of the particles to form gravitationally bound clusters with masses ranging from a few to several ten times the mass of the dwarf planet Ceres. Gravitationally bound clumps are observed to collide and merge at both moderate and high resolution. The collisional products form the top end of a distribution of planetesimal masses ranging from less than one Ceres mass to 35 Ceres masses. It remains uncertain whether collisions are driven by dynamical friction or underresolution of clumps.

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