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Modélisation des disques protoplanétaires
Vers une compréhension de leur évolution

Abstract : Gas and dust discs around young stars are probably the birth place of planets. Details of the evolution of such discs toward planetary systems are nevertheless not well understood. In this thesis, the dusty phase of circumstellar environments, from which planets will form, is studied with the aim to obtain quantitative contraints on the processes of disc evolution.

Present observational facilities offer the opportunity to study discs with an unprecedented level of details and bring essential information on the first steps of planet formation: dust growth by coagulation and settling toward the disc midplane. In order to interpret the observed properties of discs, we have developped a radiative transfer code which can synthetise coherently scattered light and/or thermal emission images, polarisation maps and spectral energy distributions of protoplanetary discs.

In a second step, the code was used to reproduce multi-wavelengths and multi-techniques observations of several discs surrounding T Tauri stars: IM Lup, IRAS 04158+2805 and GG Tau. A multi-parametric approach allowed us to precisely constrain discs parameters. Thus, we put quantitative constraints on grain growth and settling of dust grains, witnessing dust evolution, in two of these discs: IM Lup and GG Tau whereas analyses of the disc of IRAS 04158+2805 suggest, to the contrary, that dust has only marginally evolved in that disc.

The coupling of the radiative transfer code with a hydrodynamical code allows us to predict observational signatures of dust settling and radial migration. Applying these results to the circumbinary ring of GG Tau gives good agreement with observations and shows the potential of such kind of modeling to constrain physical processes within discs.

Finally, studies of the magnetospheric accretion process, of discs around brown dwarfs and Herbig Ae/Be stars as well as of more evolved discs (debris disks) mark the starting point of a systematic modeling of a growing number of discs in order to make statistical analyses of discs properties, at different spatial scales and as a function of the central object mass and of the evolutionnary state of the system.
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Contributor : Christophe Pinte <>
Submitted on : Wednesday, October 17, 2007 - 5:12:28 PM
Last modification on : Friday, November 6, 2020 - 4:07:01 AM
Long-term archiving on: : Tuesday, September 21, 2010 - 2:17:50 PM


  • HAL Id : tel-00180097, version 2




Christophe Pinte. Modélisation des disques protoplanétaires
Vers une compréhension de leur évolution. Astrophysique [astro-ph]. Université Joseph-Fourier - Grenoble I, 2006. Français. ⟨tel-00180097v2⟩



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