Icy Volatile Enhancements in Evolving Protoplanetary Disks

Abstract Protoplanetary disk ice lines shape a multitude of planet formation processes, setting the environmental composition through evolution. Ice line locations depend on molecular sublimation and deposition properties, but in dynamic disks where temperature and density structures change, so do the expected compositions of planets and planetesimals. In turbulent viscous disks with particle drift, thermal evolution, and desorption/adsorption, E. M. Price et al. demonstrated that the CO/H 2 O ice ratio beyond the CO ice line can become enhanced by ∼10 × . We expand on their work by incorporating additional carbon, nitrogen, and oxygen species, more particle sizes, and a broader disk parameter exploration. We find that, before ∼0.5 Myr, volatile ices are enhanced relative to H 2 O as the outer disk is desiccated by drift, while at later disk times, outward advection and volatile deposition further increase relative volatile icy enhancements beyond the evolving critical disk radius. The outcome of these combined relative icy enhancement to H 2 O mechanisms is solid C/O∼N/O∼1 beyond the hypervolatile ice lines, much higher than expected in static disks. Hypervolatiles (N 2 , CO, and CH 4 ) robustly increase to ∼100 × across the explored parameter space, while midvolatiles (CO 2 and NH 3 ) are sensitive to model choices, with enhancements ranging from ∼2 to 50 × . Together these results demonstrate that coupling disk dynamics with simple sublimation and deposition chemistry is fundamental to predicting grain, planetesimal, and planetary compositions, particularly the role of advection in redistributing volatiles across disk radii.