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Influence of growth on dust settling and migration in protoplanetary discs

Crespe, Elisabeth ; Gonzalez, Jean-Francois ; Laibe, Guillaume ; Maddison, Sarah T. ; Fouchet, Laure

In: Proceedings of the International Astronomical Union, 2010, vol. 6, no. S276, p. 405-406

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    Titre
    • Influence of growth on dust settling and migration in protoplanetary discs
    Auteur
    • Crespe, Elisabeth. 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. email: elisabeth.crespe@ens-lyon.fr; jean-francois.gonzalez@ens-lyon.fr
    • Gonzalez, Jean-Francois. 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. email: elisabeth.crespe@ens-lyon.fr; jean-francois.gonzalez@ens-lyon.fr
    • Laibe, Guillaume. Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Clayton Vic 3168, Australia.
    • Maddison, Sarah T.. Centre for Astrophysics and Supercomputing, Swinburne University, PO Box 218, Hawthorn, VIC 3122, Australia.
    • Fouchet, Laure. Physikalisches Institut, Universität Bern, CH-3012 Bern, Switzerland.
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Proceedings of the International Astronomical Union, 2010, vol. 6, no. S276, p. 405-406. Cambridge University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:297056
    Summary
    To form meter-sized pre-planetesimals in protoplanetary discs, dust aggregates have to decouple from the gas at a distance far enough from the central star so they are not accreted. Dust grains are affected by gas drag, which results in a vertical settling towards the mid-plane, followed by radial migration. To have a better understanding of the influence of growth on the dust dynamics, we use a simple grain growth model to determine the dust distribution in observed discs. We implement a constant growth rate into a gas+dust hydrodynamics SPH code and vary the growh rate to study the resulting effect on dust distribution. The growth rate allows us to determine the relative importance between friction and growth.We show that depending on the growth rate, a range of dust distribution can result. For large enough growth rates, grains can decouple from the gas before being accreted onto the central star, thus contributing as planetary building rocks