Dust distribution in protoplanetary disks - Vertical settling and radial migration

Details Dust distribution in protoplanetary disks - Vertical settling and radial migration Dust distribution in protoplanetary disks - Vertical settling and radial migration

2005-08-22

arxiv.org/abs/astro-ph/0508452v1

Astron.Astrophys.443:185,2005

Astronomy and Astrophysics

Astrophysics

Accepted for publication in Astronomy & Astrophysics. 11 pages, 6 figures

Scientific paper

10.1051/0004-6361:20042249

We present the results of a three dimensional, locally isothermal, non-self-gravitating SPH code which models protoplanetary disks with two fluids: gas and dust. We ran simulations of a 1 Msun star surrounded by a 0.01 Msun disk comprising 99% gas and 1% dust in mass and extending from 0.5 to ~300 AU. The grain size ranges from 0.001 mm to 10 m for the low resolution (~25 000 SPH particles) simulations and from 0.1 mm to 10 cm for the high resolution (~160 000 SPH particles) simulations. Dust grains are slowed down by the sub-Keplerian gas and lose angular momentum, forcing them to migrate towards the central star and settle to the midplane. The gas drag efficiency varies according to the grain size, with the larger bodies being weakly influenced and following marginally perturbed Keplerian orbits, while smaller grains are strongly coupled to the gas. For intermediate sized grains, the drag force decouples the dust and gas, allowing the dust to preferentially migrate radially and efficiently settle to the midplane. The resulting dust distributions for each grain size will indicate, when grain growth is added, the regions when planets are likely to form.

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