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Formation of the first planetesimals remains an unsolved problem. Growth bysticking must initiate the process, but multiple studies have revealed a seriesof barriers that can slow or stall growth, most of them due to nebulaturbulence. In a companion paper, we study the influence of these barriers onmodels of fractal aggregate and solid, compact particle growth in a viscouslyevolving solar-like nebula for a range of turbulent intensities$\alpha_{\rm{t}} = 10^{-5}-10^{-2}$. Here, we examine how disk composition inthese same models changes with time. We find that advection and diffusion ofsmall grains and vapor, and radial inward drift for larger compact particlesand fractal aggregates, naturally lead to diverse outcomes for planetesimalcomposition. Larger particles can undergo substantial inward radial migrationdue to gas drag before being collisionally fragmented or partially evaporatingat various temperatures. This leads to enhancement of the associated volatilein both vapor inside, and solids outside, their respective evaporation fronts,or ``snowlines''. In cases of lower $\alpha_{\rm{t}}$, we see narrow belts ofvolatile or supervolatile material develop in the outer nebula, which could beconnected to the bands of ``pebbles" seen by ALMA. Volatile bands, whichmigrate inwards as the disk cools, can persist over long timescales as theirgas phase continues to advect or diffuse outward across its evaporation front.These belts could be sites where supervolatile-rich planetesimals form, such asthe rare CO-rich and water-poor comets; giant planets formed just outside theH$_2$O snowline may be enhanced in water.

Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. III. Redistribution of Refractories and Volatiles