Establishing Dust Rings and Forming Planets within Them

Radio images of protoplanetary disks demonstrate that dust grains tend to organize themselves into rings. These rings may be a consequence trapping within gas pressure maxima wherein the local high dust-to-gas ratio is expected trigger formation planetesimals and eventually planets. We revisit behavior near perturbations enforced by planet in two-dimensional, shearing box simulations. While collect generally long-lived rings, particles with small Stokes parameter $\tau_s < 0.1$ advect out ring few drift timescales. Scaled properties ALMA disks, we find composed larger ($\tau_s \geq 0.1$) can nucleate clump massive enough pebble accretion which proceeds ingest entire well $\sim$1 Myr. To ensure survival favor non-planetary origin typical grain size \lesssim 0.05$--0.1. Planet-driven still possible but if so would expect orbital distance for older systems.