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• W2417526119 endingPage "3295" @default.
• W2417526119 startingPage "3274" @default.
• W2417526119 abstract "We present a model of the early chemical composition and elemental abundances of planetary atmospheres based on the cumulative gaseous chemical species that are accreted onto planets forming by core accretion from evolving protoplanetary disks. The astrochemistry of the host disk is computed using an ionization driven, non-equilibrium chemistry network within viscously evolving disk models. We accrete gas giant planets whose orbital evolution is controlled by planet traps using the standard core accretion model and track the chemical composition of the material that is accreted onto the protoplanet. We choose a fiducial disk model and evolve planets in 3 traps - water ice line, dead zone and heat transition. For a disk with a lifetime of 4.1 Myr we produce two Hot Jupiters (M = 1.43, 2.67 M$_{rm Jupiter}$, r = 0.15, 0.11 AU) in the heat transition 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 CO and H$_2$O of $1.99times 10^{-4}$, $5.0times 10^{-4}$ respectively for both Hot Jupiters. Additionally for these planets we find CO$_2$ and CH$_4$, with mixing ratios of $1.8times 10^{-6}rightarrow 9.8times 10^{-10}$ and $1.1times 10^{-8}rightarrow 2.3times 10^{-10}$ respectively. These ranges correspond well with the mixing ratio ranges that have been inferred through the detection of emission spectra from Hot Jupiters by multiple authors. We compute a carbon-to-oxygen ratio of 0.227 for the ice line planet and 0.279 for the heat transition planet. These planets accreted their gas inside the ice line, hence the sub-solar C/O." @default.
• W2417526119 created "2016-06-24" @default.
• W2417526119 creator A5020298532 @default.
• W2417526119 creator A5042081134 @default.
• W2417526119 creator A5055513962 @default.
• W2417526119 date "2016-06-24" @default.
• W2417526119 modified "2023-09-23" @default.
• W2417526119 title "Composition of early planetary atmospheres – I. Connecting disc astrochemistry to the formation of planetary atmospheres" @default.
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