Chemical enrichment of giant planets and discs due to pebble drift

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This work has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG.

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H2O abundances and cloud properties in ten hot giant exoplanets (2018, background): “Alternatively, some of the hot Jupiters may have formed through pebble accretion and migrated inward with or without the disk but without significant erosion of the core (Madhusudhan et al. 2017; Booth et al. 2017).”
Equilibrium chemistry down to 100 K (2017, background): “Such effects are rarely studied in detail (see, however, Booth et al. 2017).”
Mass–Metallicity Trends in Transiting Exoplanets from Atmospheric Abundances of H2O, Na, and K (2019, background): “Another possibility is the formation of giant planets by accreting metal-rich and high C/O gas caused by pebble drift (Öberg & Bergin 2016; Booth et al. 2017).”
Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects (2019, background): “The circles denote planets formed by pebble accretion, taking into account the chemical evolution driven by pebble migration (31).”
Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST (2017, background): “In particular, measuring the abundances of molecular species in the atmospheres of a diverse range of planets may reveal how the atmosphere was accreted or outgassed, and how it subsequently evolved (Oberg et al. 2011; Booth et al. 2017; Espinoza et al. 2017).”