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The similar orbital distances and detection rates of debris disks and theprominent rings observed in protoplanetary disks suggest a potential connectionbetween these structures. We explore this connection with new calculations thatfollow the evolution of rings of pebbles and planetesimals as they grow intoplanets and generate dusty debris. Depending on the initial solid mass andplanetesimal formation efficiency, the calculations predict diverse outcomesfor the resulting planet masses and accompanying debris signature. Whencompared with debris disk incidence rates as a function of luminosity and time,the model results indicate that the known population of bright cold debrisdisks can be explained by rings of solids with the (high) initial massesinferred for protoplanetary disk rings and modest planetesimal formationefficiencies that are consistent with current theories of planetesimalformation. These results support the possibility that large protoplanetary diskrings evolve into the known cold debris disks. The inferred strong evolutionaryconnection between protoplanetary disks with large rings and mature stars withcold debris disks implies that the remaining majority population of low-massstars with compact protoplanetary disks leave behind only modest masses ofresidual solids at large radii and evolve primarily into mature stars withoutdetectable debris beyond 30 au. The approach outlined here illustrates howcombining observations with detailed evolutionary models of solids stronglyconstrains the global evolution of disk solids and underlying physicalparameters such as the efficiency of planetesimal formation and the possibleexistence of invisible reservoirs of solids in protoplanetary disks.

From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection