  Dust particles in protoplanetary disks, lacking support from pressure, rotate
at velocities exceeding those of the surrounding gas. Consequently, they
experience a head-wind from the gas that drives them toward the central star.
Radial drift occurs on timescales much shorter than those inferred from disk
observations or those required for dust to aggregate and form planets.
Additionally, turbulence is often assumed to amplify the radial drift of dust
in planet-forming disks when modeled through an effective viscous transport.
However, the local interactions between turbulent eddies and particles are
known to be significantly more intricate than in a viscous fluid. Our objective
is to elucidate and characterize the dynamic effects of Keplerian turbulence on
the mean radial and azimuthal velocities of dust particles. We employ 2D
shearing-box incompressible simulations of the gas, which is maintained in a
developed turbulent state while rotating at a sub-Keplerian speed. Dust is
modeled as Lagrangian particles set at a Keplerian velocity, therefore
experiencing a radial force toward the star through drag. Turbulent eddies are
found to reduce the radial drift, while simultaneously enhancing the azimuthal
velocities of small particles. This dynamic behavior arises from the
modification of dust trajectories due to turbulent eddies.
