Tracing Resonant Planetary Migration Signatures in Protoplanetary and Debris Disks

Planetary systems observed near mean-motion resonances offer a unique window into the conditions of their formation and early evolution. While much work has focused on their protoplanetary phase, the potential imprint of resonant migration on debris disks remains mostly unexplored. In this work, we investigate how the dynamical interaction between resonant planets and the remnant planetesimal population can shape debris disk morphology, particularly when the system has undergone outward migration.

We use high-resolution hydrodynamical simulations with the PLUTO code, including Lagrangian particles to represent a broad range of dust and planetesimal sizes. These particles are evolved in the presence of migrating resonant planet pairs that open a common gap in the disk. As the planets migrate inward/outward, a dusty ring will build-up at the gap outer edge and it will tag along the planets, imprinting the dust distribution at the end of the protoplanetary disk lifetime. We follow up the disk dispersal and long term evolution of the planetesimal using the N-body code Rebound.

We then explore how the resonant migration is affecting the observable disk structures by generating synthetic observations to assess the detectability of these features both in Class II and III disks.