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Influence of growth on dust settling and migration in protoplanetary discs

Published online by Cambridge University Press:  10 November 2011

Elisabeth Crespe
Affiliation:
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
Jean-Francois Gonzalez
Affiliation:
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
Guillaume Laibe
Affiliation:
Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Clayton Vic 3168, Australia.
Sarah T. Maddison
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University, PO Box 218, Hawthorn, VIC 3122, Australia.
Laure Fouchet
Affiliation:
Physikalisches Institut, Universität Bern, CH-3012 Bern, Switzerland.
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Abstract

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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Barrière-Fouchet, L., Gonzalez, J.-F., Murray, J. R., Humble, R. J., & Maddison, S. T. 2005, A&A, 443, 185Google Scholar
Laibe, G., Gonzalez, J.-F., Fouchet, L., & Maddison, S. T. 2008, A&A, 487, 265Google Scholar
Laibe, G., Gonzalez, J.-F., & Maddison, S. T. 2010a, A&A, under revision after referee's reportGoogle Scholar
Laibe, G., Gonzalez, J.-F., Maddison, S. T., Crespe, E., & Fouchet, L. 2010b, A&A, submittedGoogle Scholar
Stepinski, T. F., & Valageas, P., 1997, A&A, 319, 1007Google Scholar

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