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Understanding the origin of accretion and dispersal of protoplanetary disksis fundamental for investigating planet formation. Recent numerical simulationsshow that launching winds are unavoidable when disks undergo magneticallydriven accretion and/or are exposed to external UV radiation. Observations alsohint that disk winds are common. We explore how the resulting wind mass lossrate can be used as a probe of both disk accretion and dispersal. As aproof-of-concept study, we focus on magnetocentrifugal winds, MRI(magnetorotational instability) turbulence, and external photoevapotaion. Bydeveloping a simple, yet physically motivated disk model and coupling it withsimulation results available in the literature, we compute the mass loss rateas a function of external UV flux for each mechanism. We find that differentmechanisms lead to different levels of mass loss rate, indicating that theorigin of disk accretion and dispersal can be determined, by observing the windmass loss rate resulting from each mechanism. This determination providesimportant implications for planet formation. This work thus shows that theongoing and future observations of the wind mass loss rate for protoplanetarydisks are paramount to reliably constrain how protoplanetary disks evolve withtime and how planet formation takes place in the disks.

Determining dispersal mechanisms of protoplanetary disks using accretion and wind mass loss rates