Effect of turbulence on collisions of dust particles with planetesimals in protoplanetary disks

• Published in: Astronomy and astrophysics (Berlin) Vol. 589; p. A129
• Main Authors: Homann, H., Guillot, T., Bec, J., Ormel, C. W., Ida, S., Tanga, P.
• Format: Journal Article
• Language: English
• Published: EDP Sciences 01.05.2016
• Subjects: accretion; accretion disks; Astrophysics; Collision rates; Collisions; Computational fluid dynamics; Data Analysis, Statistics and Probability; Dust; Earth and Planetary Astrophysics; Earth Sciences; Geophysics; hydrodynamics; Instrumentation and Methods for Astrophysic; Mathematical models; methods: numerical; Physics; Planet formation; planet-disk interactions; Planetology; planets and satellites: formation; Sciences of the Universe; Space Physics; Turbulence; Turbulent flow
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/201527344

Context. Planetesimals in gaseous protoplanetary disks may grow by collecting dust particles. Hydrodynamical studies show that small particles generally avoid collisions with the planetesimals because they are entrained by the flow around them. This occurs when St, the Stokes number, defined as the ratio of the dust stopping time to the planetesimal crossing time, becomes much smaller than unity. However, these studies have been limited to the laminar case, whereas these disks are believed to be turbulent. Aims. We want to estimate the influence of gas turbulence on the dust-planetesimal collision rate and on the impact speeds. Methods. We used three-dimensional direct numerical simulations of a fixed sphere (planetesimal) facing a laminar and turbulent flow seeded with small inertial particles (dust) subject to a Stokes drag. A no-slip boundary condition on the planetesimal surface is modeled via a penalty method. Results. We find that turbulence can significantly increase the collision rate of dust particles with planetesimals. For a high turbulence case (when the amplitude of turbulent fluctuations is similar to the headwind velocity), we find that the collision probability remains equal to the geometrical rate or even higher for St ≳ 0.1, i.e., for dust sizes an order of magnitude smaller than in the laminar case. We derive expressions to calculate impact probabilities as a function of dust and planetesimal size and turbulent intensity.