  The disk midplane temperature is potentially affected by the dust
traps/rings. The dust depletion beyond the water snowline will cast a shadow.
In this study, we adopt a detailed gas-grain chemical reaction network, and
investigate the radial gas and ice abundance distributions of dominant carbon-,
oxygen-, and nitrogen-bearing molecules in disks with shadow structures beyond
the water snowline around a protosolar-like star. In shadowed disks, the dust
grains at around $3-8$ au are predicted to have more than around $5-10$ times
amounts of ices of organic molecules such as H$_{2}$CO, CH$_{3}$OH, and
NH$_{2}$CHO, saturated hydrocarbon ices such as CH$_{4}$ and C$_{2}$H$_{6}$, in
addition to H$_{2}$O, CO, CO$_{2}$, NH$_{3}$, N$_{2}$, and HCN ices, compared
with those in non-shadowed disks. In the shadowed regions, we find that
hydrogenation (especially of CO ice) is the dominant formation mechanism of
complex organic molecules. The gas-phase N/O ratios show much larger spatial
variations than the gas-phase C/O ratios, thus the N/O ratio is predicted to be
a useful tracer of the shadowed region. N$_{2}$H$^{+}$ line emission is a
potential tracer of the shadowed region. We conclude that a shadowed region
allows the recondensation of key volatiles onto dust grains, provides a region
of chemical enrichment of ices that is much closer to the star than within a
non-shadowed disk, and may explain to some degree the trapping of O$_{2}$ ice
in dust grains that formed comet 67P/Churyumov-Gerasimenko. We discuss that, if
formed in a shadowed disk, Jupiter does not need to have migrated vast
distances.
