Induced Turbulence and the Density Structure of the Dust Layer in a Protoplanetary Disk
Abstract
We study the turbulence induced in the dust layer of a protoplanetary disk based on the energetics of dust accretion due to gas drag. We estimate turbulence strength from the energy supplied by dust accretion, using the radial drift velocity of the dust particles in a laminar disk. Our estimate of the turbulence strength agrees with previous analytical and numerical research on the turbulence induced by Kelvin-Helmholtz and/or streaming instabilities for particles with stopping time less than the Keplerian time. For such small particles, the strongest turbulence is expected to occur when the dust-to-gas ratio of the disk is ~C 1/2 eff(hg /r) ~ 10-2, where C eff ≈ 0.2 represents the energy supply efficiency to turbulence and hg /r ~ 5 × 10-2 is the aspect ratio of the gas disk. The maximum viscosity parameter is αmax ~ C eff Ts (hg /r)2 ~ 10-4 Ts , where Ts (< 1) is the non-dimensional stopping time of the dust particles. Modification to the dust-to-gas ratio from the standard value, 10-2, by any process, results in weaker turbulence and a thinner dust layer, and consequently may accelerate the growth process of the dust particles.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- January 2012
- DOI:
- 10.1088/0004-637X/744/2/101
- arXiv:
- arXiv:1109.4755
- Bibcode:
- 2012ApJ...744..101T
- Keywords:
-
- accretion;
- accretion disks;
- planets and satellites: formation;
- protoplanetary disks;
- Astrophysics - Earth and Planetary Astrophysics
- E-Print:
- Accepted in ApJ (18 pages, 11 figures)