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Over one quarter of white dwarfs contain observable metallic debris from thebreakup of exo-asteroids. Understanding the physical and orbital history ofthis debris would enable us to self-consistently link planetary systemformation and fate. One major debris reservoir is generated by YORP-inducedrotational fission during the giant branch phases of stellar evolution, wherethe stellar luminosity can exceed the Sun's by four orders of magnitude. Here,we determine the efficacy of the giant branch YORP effect for asteroids withnonzero internal strength, and model post-fission evolution by imposing simpleanalytic fragmentation prescriptions. We find that even the highest realisticinternal strengths cannot prevent the widespread fragmentation of asteroids andthe production of a debris field over 100 au in size. We compute the number ofsuccessive fission events as they occur in progressively smaller time intervalsas the star ascends the giant branches, providing a way to generate sizedistributions of asteroid fragments. The results are highly insensitive toprogenitor stellar mass. We also conclude that the ease with which giant branchYORP breakup can generate binary asteroid subsystems is strongly dependent oninternal strength. Formed binary subsystems in turn could be short-lived due tothe resulting luminosity-enhanced BYORP effect.

Post-main-sequence debris from rotation-induced YORP break-up of small bodies II: multiple fissions, internal strengths and binary production