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• W4288925041 abstract "ABSTRACT The atmospheric chemical composition of a hot Jupiter can lead to insights into where in its natal protoplanetary disc it formed and its subsequent migration pathway. We use a 1D chemical kinetics code to compute a suite of models across a range of elemental abundances to investigate the resultant abundances of key molecules in hot Jupiter atmospheres. Our parameter sweep spans metallicities between 0.1x and 10x solar values for the C/H, O/H, and N/H ratios, and equilibrium temperatures of 1000 and 2000 K. We link this parameter sweep to the formation and migration models from previous works to predict connections between the atmospheric molecular abundances and formation pathways, for the molecules H2O, CO, CH4, CO2, HCN, and NH3. We investigate atmospheric H2O abundances in eight hot Jupiters reported in the literature. All eight planets fall within our predicted ranges for various formation models; however, six of them are degenerate between multiple models and hence require additional molecular detections for constraining their formation histories. The other two planets, HD 189733 b and HD 209458 b, have water abundances that fall within ranges expected from planets that formed beyond the CO2 snowline. Finally, we investigate the detections of H2O, CO, CH4, CO2, HCN, and NH3 in the atmosphere of HD 209458 b and find that, within the framework of our model, the abundances of these molecules best match with a planet that formed between the CO2 and CO snowlines and then underwent disc-free migration to reach its current location." @default.
• W4288925041 created "2022-07-31" @default.
• W4288925041 creator A5013679577 @default.
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• W4288925041 date "2022-07-31" @default.
• W4288925041 modified "2023-10-15" @default.
• W4288925041 title "Molecular tracers of planet formation in the atmospheres of hot Jupiters" @default.
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• W4288925041 doi "https://doi.org/10.1093/mnras/stac2106" @default.
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