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A key challenge for protoplanetary disks and planet formation models is to beable to make a reliable connection between observed structures in the disksemission, like bright and dark rings or asymmetries, and the supposed existenceof planets triggering these structures. The observation of N dark rings ofemission is often interpreted as evidence for the presence of N planets whichclear dust gaps around their orbit and form dust-trapping pressure maxima inthe disk. The vast majority of the models that studied the impact of planets onthe dynamics of dust and gas in a protoplanetary disk assumed planets on fixedorbits. Here we go a different route and examine how the large-scale inwardmigration of a single planet structures the dust content of a massive disk. Inmany circumstances, the migration of a partial gap-opening planet with a masscomparable to Saturn is found to run away intermittently. By means of 2D gasand dust hydrodynamical simulations, we show that intermittent runawaymigration can form multiple dust rings and gaps across the disk. Each timemigration slows down, a pressure maximum forms beyond the planet gap that trapsthe large dust. Post-processing of our simulations results with 3D dustradiative transfer calculations confirms that intermittent runaway migrationcan lead to the formation of multiple sets of bright and dark rings ofcontinuum emission in the (sub)millimeter beyond the planet location.

Intermittent planet migration and the formation of multiple dust rings and gaps in protoplanetary disks