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We present the next step in a series of papers devoted to connecting thecomposition of the atmospheres of forming planets with the chemistry of theirnatal evolving protoplanetary disks. The model presented here computes thecoupled chemical and dust evolution of the disk and the formation of threeplanets per disk model. Our three canonical planet traps produce a Jupiter near1 AU, a Hot Jupiter and a Super-Earth. We study the dependency of the finalorbital radius, mass, and atmospheric chemistry of planets forming in diskmodels with initial disk masses that vary by 0.02 $M_\odot$ above and below ourfiducial model ($M_{disk,0} = 0.1 ~M_\odot$). We compute C/O and C/N for theatmospheres formed in our 3 models and find that C/O$_{\rm planet}\sim$C/O$_{\rm disk}$, which does not vary strongly between different planets formedin our model. The nitrogen content of atmospheres can vary in planets that growin different disk models. These differences are related to the formationhistory of the planet, the time and location that the planet accretes itsatmosphere, and are encoded in the bulk abundance of NH$_3$. These resultssuggest that future observations of atmospheric NH$_3$ and an estimation of theplanetary C/O and C/N can inform the formation history of particular planetarysystems.

Composition of Early Planetary Atmospheres II: Coupled Dust and Chemical Evolution in Protoplanetary Disks