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We present a model of the early chemical composition and elemental abundancesof planetary atmospheres based on the cumulative gaseous chemical species thatare accreted onto planets forming by core accretion from evolvingprotoplanetary disks. The astrochemistry of the host disk is computed using anionization driven, non-equilibrium chemistry network within viscously evolvingdisk models. We accrete gas giant planets whose orbital evolution is controlledby planet traps using the standard core accretion model and track the chemicalcomposition of the material that is accreted onto the protoplanet. We choose afiducial disk model and evolve planets in 3 traps - water ice line, dead zoneand heat transition. For a disk with a lifetime of 4.1 Myr we produce two HotJupiters (M = 1.43, 2.67 M$_{\rm Jupiter}$, r = 0.15, 0.11 AU) in the heattransition and ice line trap and one failed core (M = 0.003 M$_{\rm Jupiter}$,r =3.7 AU) in the dead zone. These planets are found with mixing ratios for COand H$_2$O of $1.99\times 10^{-4}$, $5.0\times 10^{-4}$ respectively for bothHot Jupiters. Additionally for these planets we find CO$_2$ and CH$_4$, withmixing ratios of $1.8\times 10^{-6}\rightarrow 9.8\times 10^{-10}$ and$1.1\times 10^{-8}\rightarrow 2.3\times 10^{-10}$ respectively. These rangescorrespond well with the mixing ratio ranges that have been inferred throughthe detection of emission spectra from Hot Jupiters by multiple authors. Wecompute a carbon-to-oxygen ratio of 0.227 for the ice line planet and 0.279 forthe heat transition planet. These planets accreted their gas inside the iceline, hence the sub-solar C/O.

Composition of Early Planetary Atmospheres I: Connecting Disk Astrochemistry to the Formation of Planetary Atmospheres