We present the next step in a series of papers devoted to connecting the
composition of the atmospheres of forming planets with the chemistry of their
natal evolving protoplanetary disks. The model presented here computes the
coupled chemical and dust evolution of the disk and the formation of three
planets per disk model. Our three canonical planet traps produce a Jupiter near
1 AU, a Hot Jupiter and a Super-Earth. We study the dependency of the final
orbital radius, mass, and atmospheric chemistry of planets forming in disk
models with initial disk masses that vary by 0.02 Mββ above and below our
fiducial model (Mdisk,0β=0.1Β Mββ). We compute C/O and C/N for the
atmospheres formed in our 3 models and find that C/OplanetββΌ
C/Odiskβ, which does not vary strongly between different planets formed
in our model. The nitrogen content of atmospheres can vary in planets that grow
in different disk models. These differences are related to the formation
history of the planet, the time and location that the planet accretes its
atmosphere, and are encoded in the bulk abundance of NH3β. These results
suggest that future observations of atmospheric NH3β and an estimation of the
planetary C/O and C/N can inform the formation history of particular planetary
systems.Comment: Accepted for publication in MNRA