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Title:
Dust evolution in protoplanetary disks
Authors:
Gonzalez, Jean-François; Fouchet, Laure; Maddison, Sarah T.; Laibe, Guillaume
Affiliation:
AA(Université de Lyon, Lyon, F-69003, France; Université Lyon 1, Villeurbanne, F-69622, France; CNRS, UMR 5574, Centre de Recherche Astrophysique de Lyon, École Normale Supérieure de Lyon, 46 allée d'Italie, F-69364 Lyon cedex 07, France ), AB(Department of Physics, ETH Zürich, CH-8093 Zürich, Switzerland ), AC(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia ), AD(Université de Lyon, Lyon, F-69003, France; Université Lyon 1, Villeurbanne, F-69622, France; CNRS, UMR 5574, Centre de Recherche Astrophysique de Lyon, École Normale Supérieure de Lyon, 46 allée d'Italie, F-69364 Lyon cedex 07, France )
Publication:
Exoplanets: Detection, Formation and Dynamics, Proceedings of the International Astronomical Union, IAU Symposium, Volume 249, p. 375-380
Publication Date:
05/2008
Origin:
CUP
Keywords:
planetary systems: protoplanetary disks – hydrodynamics – methods: numerical
DOI:
10.1017/S1743921308016840
Bibliographic Code:
2008IAUS..249..375G

Abstract

We investigate the behaviour of dust in protoplanetary disks under the action of gas drag using our 3D, two-fluid (gas+dust) SPH code. We present the evolution of the dust spatial distribution in global simulations of planetless disks as well as of disks containing an already formed planet. The resulting dust structures vary strongly with particle size and planetary gaps are much sharper than in the gas phase, making them easier to detect with ALMA than anticipated. We also find that there is a range of masses where a planet can open a gap in the dust layer whereas it doesn't in the gas disk. Our dust distributions are fed to the radiative transfer code MCFOST to compute synthetic images, in order to derive constraints on the settling and growth of dust grains in observed disks.
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