Dispersal of protoplanetary disks by central wind stripping
arXiv:0904.3363 · doi:10.1088/0004-637X/700/1/10
Abstract
We present a model for the dispersal of protoplanetary disks by winds from either the central star or the inner disk. These winds obliquely strike the flaring disk surface and strip away disk material by entraining it in an outward radial-moving flow at the wind-disk interface which lies several disk scale heights above the mid-plane. The disk dispersal time depends on the entrainment velocity at which disk material flows into this turbulent shear layer interface. If the entrainment efficiency is ~10% of the local sound speed, a likely upper limit, the dispersal time at 1 AU is ~6 Myr for a disk with a surface density of 10^3 g cm^{-2}, a solar mass central star, and a wind with an outflow rate 10^{-8} Msun/yr and terminal velocity 200 km/s. When compared to photoevaporation and viscous evolution, wind stripping can be a dominant mechanism only for the combination of low accretion rates (< 10^{-8} Msun/yr) and wind outflow rates approaching these accretion rates. This case is unusual since generally outflow rates are < 0.1 of of accretion rates.
12 pages, 9 figures, accepted for publication in ApJ
References in corpus (5)
- Photoevaporation of protoplanetary discs II: evolutionary models and observable properties
- Photoevaporation of protoplanetary discs I: hydrodynamic models
- Line Emission from Gas in Optically Thick Dust Disks around Young Stars
- c2d Spitzer IRS Spectra of Disks around T Tauri Stars. III. [Ne II], [Fe I], and H_2 gas-phase lines
- Neon Fine-Structure Line Emission By X-ray Irradiated Protoplanetary Disks
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