  Super-Earths can form at large orbital radii and migrate inward due to tidal
interactions with the circumstellar disk. In this scenario, convergent
migration may occur and lead to the formation of resonant pairs of planets. We
explore the conditions under which convergent migration and resonance capture
take place, and what dynamical consequences can be expected on the dust
distribution surrounding the resonant pair. We combine hydrodynamic
planet--disk interaction models with dust evolution calculations to investigate
the signatures produced in the dust distribution by a pair of planets in
mean-motion resonances. We find that convergent migration takes place when the
outer planet is the more massive. However, convergent migration also depends on
the local properties of the disk, and divergent migration may result as well.
For similar disk parameters, the capture in low degree resonances (e.g., 2:1 or
3:2) is preferred close to the star where the resonance strength can more
easily overcome the tidal torques exerted by the gaseous disk. Farther away
from the star, convergent migration may result in capture in high degree
resonances. The dust distribution shows potentially observable features
typically when the planets are trapped in a 2:1 resonance. In other cases, with
higher degree resonances (e.g., 5:4 or 6:5) dust features may not be
sufficiently pronounced to be easily observable. The degree of resonance
established by a pair of super-Earths may be indicative of the location in the
disk where capture occurred. There can be significant differences in the dust
distribution around a single super-Earth and a pair of super-Earths in
resonance.
