  The supersolar abundances of volatiles observed in giant planets suggest that
a compositional gradient was present at the time of their formation in the
protosolar nebula. To explain this gradient, several studies have investigated
the radial transport of trace species and the effect of icelines on the
abundance profiles of solids and vapors formed in the disk. However, these
models only consider the presence of solids in the forms of pure condensates or
amorphous ice during the evolution of the protosolar nebula. They usually
neglect the possible crystallization and destabilization of clathrates, along
with the resulting interplay between the abundance of water and those of these
crystalline forms. This study is aimed at pushing this kind of investigation
further by considering all possible solid phases together in the protosolar
nebula: pure condensates, amorphous ice, and clathrates. To this end, we used a
one-dimensional (1D) protoplanetary disk model coupled with modules describing
the evolution of trace species in the vapor phase, as well as the dynamics of
dust and pebbles. Eleven key species are considered here, including H$_2$O, CO,
CO$_2$, CH$_4$, H$_2$S, N$_2$, NH$_3$, Ar, Kr, Xe, and PH$_3$. Two sets of
initial conditions are explored for the protosolar nebula. In a first scenario,
the disk is initially filled with icy grains in the forms of pure condensates.
In this case, we show that clathrates can crystallize and form enrichment peaks
up to about ten times the initial abundances at their crystallization lines. In
a second scenario, the volatiles were delivered to the protosolar nebula in the
forms of amorphous grains. In this case, the presence of clathrates is not
possible because there is no available crystalline water ice in their formation
region. Enrichment peaks of pure condensates also form beyond the snowline up
to about seven times the initial abundances.
