Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
Andrew N. Youdin, Yoram Lithwick (CITA)

TL;DR
This paper derives a new formula for particle diffusion in turbulent gas disks, accounting for orbital oscillations, which impacts particle settling and potential planetesimal formation.
Contribution
It introduces a corrected Schmidt number formula incorporating orbital dynamics, improving understanding of particle diffusion in protoplanetary disks.
Findings
Schmidt number scales quadratically with stopping time
Particles larger than ~10 cm settle closer to the midplane
Vertical particle velocities and scale heights are confirmed and refined
Abstract
We describe the diffusion and random velocities of solid particles due to stochastic forcing by turbulent gas. We include the orbital dynamics of Keplerian disks, both in-plane epicycles and vertical oscillations. We obtain a new result for the diffusion of solids. The Schmidt number (ratio of gas to particle diffusivity) is Sc = 1 + (Omega t_stop)^2, in terms of the particle stopping time, t_stop, and the orbital frequency, Omega. The standard result, Sc = 1 + t_stop/t_eddy, in terms of the eddy turnover time, t_eddy, is shown to be incorrect. The main difference is that Sc rises quadratically, not linearly, with stopping time. Consequently, particles larger than ~ 10 cm in protoplanetary disks will suffer less radial diffusion and will settle closer to the midplane. Such a layer of boulders would be more prone to gravitational collapse. Our predictions of RMS speeds, vertical scale…
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