  The abundances of volatile CHNOS have a profound effect on the interior
structure and evolution of a planet. Therefore, it is key to investigate the
behavior of the abundances of these elements in the solid phase in the earliest
stages of planet formation. However, the processes in planet-forming disks that
shape these abundances are highly coupled and nonlocal. We aim to quantify the
effects of the interplay between dynamical, collision, ice processing on the
abundances of CHNOS in local disk solids as a function of position throughout
the planet-forming region. We used SHAMPOO (StocHAstic Monomer PrOcessOr),
which tracks the ice budgets of CHNOS-bearing molecules of a dust monomer as it
undergoes nonlocal disk processing in a Class I disk. We used a large set of
individual monomer evolutionary trajectories to make inferences about the
properties of the local dust populations. We find that spatially, monomers can
travel larger distances farther out in the disk, leading to a larger spread in
positions of origin for a dust population at, for example, r=50 AU compared to
r=2 AU. However, chemically, the inner disk (r<10 AU) is more nonlocal due to
the closer spacing of ice lines in this disk region. We find that the ice mass
associated with individual chemical species can change significantly. The
largest differences with local dust were found near ice lines where the
collisional timescale is comparable to the adsorption and desorption
timescales. Here, aggregates may become significantly depleted in ice as a
consequence of microscopic collisional mixing, a previously unknown effect
where monomers are stored away in aggregate interiors through rapid cycles of
coagulation and fragmentation. This suggests that ice processing is highly
coupled to collisional processing in this disk region, which implies that the
interiors of dust aggregates must be considered and not just their surfaces.
