Hostname: page-component-6bf8c574d5-7jkgd Total loading time: 0 Render date: 2025-02-23T05:18:41.298Z Has data issue: false hasContentIssue false
  • English
  • Français

3D SPH simulations of grain growth in protoplanetary disks

Published online by Cambridge University Press:  01 October 2007

Guillaume Laibe ,
Jean-François Gonzalez ,
Laure Fouchet  and
Sarah T. Maddison
Guillaume Laibe
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: [email protected], [email protected]
Jean-François 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: [email protected], [email protected]
Laure Fouchet
Affiliation:
Department of Physics, ETH Zurich, CH-8093 Zurich, Switzerland email: [email protected]
Sarah T. Maddison
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the first results of the treatment of grain growth in our 3D, two-fluid (gas+dust) SPH code describing protoplanetary disks. We implement a scheme able to reproduce the variation of grain sizes caused by a variety of physical processes and test it with the analytical expression of grain growth given by Stepinski & Valageas (1997) in simulations of a typical T Tauri disk around a one solar mass star. The results are in agreement with a turbulent growing process and validate the method. We are now able to simulate the grain growth process in a protoplanetary disk given by a more realistic physical description, currently under development. We discuss the implications of the combined effect of grain growth and dust vertical settling and radial migration on subsequent planetesimal formation.

Keywords

planetary systems: protoplanetary disks — hydrodynamics — methods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 385 - 388
Copyright
Copyright © International Astronomical Union 2008

References

Apai, D., Pascucci, I., Sterzik, M. F., et al. 2004, A&A, 426, L53Google Scholar
Barrière-Fouchet, L., Gonzalez, J.-F., Murray, J. R., Humble, R. J., & Maddison, S. T. 2005, A&A, 443, 185Google Scholar
Dominik, C., Tielens, A. G. G. M. 1997, ApJ, 480, 647CrossRefGoogle Scholar
Dullemond, C. P. & Dominik, C. 2005, A&A, 434, 971Google Scholar
Fouchet, L., Maddison, S. T., Gonzalez, J.-F., & Murray, J. R. 2007, A&A, in press (arXiv:0708.4110)Google Scholar
Maddison, S. T., Fouchet, L., & Gonzalez, J.-F. 2007, Ap&SS, 474, 1037Google Scholar
Pinte, C., Fouchet, L., Ménard, F., Gonzalez, J.-F., & Duchêne, G. 2007, A&A, 469, 963Google Scholar
Price, D. 2007, PASA, accepted (arXiv:0709.0832)Google Scholar
Shakura, N. I. & Sunyaev, R. A. 1973, A&A, 24, 337Google Scholar
Stepinski, T. F. & Valageas, P. 1997, A&A, 319, 1007Google Scholar