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Planet migration in protoplanetary discs plays an important role in thelonger term evolution of planetary systems, yet we currently have no directobservational test to determine if a planet is migrating in its gaseous disc.We explore the formation and evolution of dust rings - now commonly observed inprotoplanetary discs by ALMA - in the presence of relatively low mass (12-60Earth masses) migrating planets. Through two dimensional hydrodynamicalsimulations using gas and dust we find that the importance of perturbations inthe pressure profile interior and exterior to the planet varies for differentparticle sizes. For small sizes a dust enhancement occurs interior to theplanet, whereas it is exterior to it for large particles. The transitionbetween these two behaviours happens when the dust drift velocity is comparableto the planet migration velocity. We predict that an observational signature ofa migrating planet consists of a significant outwards shift of an observedmidplane dust ring as the wavelength is increased.

Is the ring inside or outside the planet?: The effect of planet migration on dust rings