Sign on
ADS Classic is now deprecated. It will be completely retired in October 2019. This page will automatically redirect to the new ADS interface at that point.

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Printable Article (PDF/Postscript)
· Scanned Article (GIF)
· Table of Contents
· References in the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
High-resolution simulations of planetesimal formation in turbulent protoplanetary discs
Authors:
Johansen, Anders; Klahr, Hubert; Henning, Thomas
Affiliation:
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)
Publication:
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:
11/2011
Origin:
CUP
Keywords:
accretion, accretion disks, MHD, turbulence, planetary systems: formation, planetary systems: protoplanetary disks
Abstract Copyright:
(c) 2011: Copyright © International Astronomical Union 2011
DOI:
10.1017/S1743921311019995
Bibliographic Code:
2011IAUS..276...89J

Abstract

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.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints