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High-resolution simulations of planetesimal formation in turbulent protoplanetary discs

Published online by Cambridge University Press:  10 November 2011

Anders Johansen ,
Hubert Klahr  and
Thomas Henning
Anders Johansen
Affiliation:
Lund Observatory, Lund University, Box 43, 221 00 Lund, Sweden email: anders@astro.lu.se
Hubert Klahr
Affiliation:
Max-Planck-Institut für Astronomie Königstuhl 17, 69117 Heidelberg, Germany
Thomas Henning
Affiliation:
Max-Planck-Institut für Astronomie Königstuhl 17, 69117 Heidelberg, Germany
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Abstract

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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.

Keywords

accretionaccretion disksMHDturbulenceplanetary systems: formationplanetary systems: protoplanetary disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 89 - 94
Copyright
Copyright © International Astronomical Union 2011

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