Surface density of pebbles, Σ_p, near a 1.51 M_⊕ planet for three values of the Stokes number: St = 0.014, 0.089, and 0.546 (left, middle, and right columns, respectively). The black circle shows the extent of the Hill radius, and the white arrows show the direction of the shear motion relative to the planet. In an inertial frame, the planet would orbit in the y > 0 direction. Radial drift of pebbles occurs in the x < 0 direction. The lower and upper limits of the logarithmic colour palette correspond to the initial pebble surface density at the planet location multiplied by 10⁻¹ and 10¹, respectively. Top: Σ_p results directly from FARGOЗD multi-fluid simulations. The black curves are streamlines of the pebble fluid. The planetary potential smoothing for pebbles is є_p = 1 R_H, and the simulation time is t = 50 P_orb. Middle: Σ_p calculated from the distribution of superparticles by the cloud-in-cell method and averaged in time. The black curves are trajectories of individual superparticles. The potential smoothing for pebbles is є_p = 1 R_H, and the simulation time is t = 200 P_orb. Bottom: as in the middle row but avoiding potential smoothing for pebbles and allowing for pebble accretion.