  In this chapter we outline some of the basic understanding of the chemistry
that accompanies planet formation. We discuss the basic physical environment
which dictates the dominant chemical kinetic pathways for molecule formation.
We focus on three zones from both observational and theoretical perspectives:
(1) the planet forming midplane and ice/vapor transition zones (snow-lines),
(2) the warm disk surface that is shielded from radiation, which can be readily
accessed by todays observational facilities, and (3) the surface
photodissociation layers where stellar radiation dominates. We end with a
discussion of how chemistry influences planet formation along with how to probe
the link between formation and ultimate atmospheric composition for gas giants
and terrestrial worlds.
