Towards measuring dust settling in protoplanetary disks

Details Towards measuring dust settling in protoplanetary disks Towards measuring dust settling in protoplanetary disks

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sf2a.conf...63b&link_type=abstract

SF2A-2004: Semaine de l'Astrophysique Francaise, meeting held in Paris, France, June 14-18, 2004. Edited by F. Combes, D. Barret

Physics

Optics

1

Scientific paper

High resolution images of a few protoplanetary disks are available over a wide wavelength range, from the optical with HST , NIR with ground-based adaptive optics, to millimeter with long-baseline interferometers. Model fitting of these images have been usually restricted to one wavelength. Attempts to simultaneously fit all wavelengths with a single model indicate that the grain size distribution is likely more complex than the simple ISM one. In particular, a dependence of the maximum grain size with vertical distance above the disk midplane (vertical settling) appears to be needed. In this contribution we present synthetic images that include more realistic vertical grain size distributions obtained from recent hydrodynamical (SPH) calculations. The calculations are three-dimensional, they include the effects of hydrodynamical forces and gas drag upon an evolving dusty gas disk. We briefly describe the numerical method. In particular, the SPH code provides vertical density profiles for the dust as a function of grain size. Radiative transfer is done with a 3D multiple scattering code to produce synthetic images in all four Stokes parameters. Comparison with observations of a sample of resolved disks will help validate the hydrodynamical simulations and to constrain grain growth and evaporation processes in these disks, a crucial step towards understanding planet formation. We present here the case of GG Tau. Such a combination of hydrodynamical and radiative transfer calculations is needed to prepare observations with future instruments like Planet Finder or ALMA.

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