English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Atmospheric chemical abundances of giant planets lead to importantconstraints on planetary formation and migration. Studies have shown that giantplanets that migrate through the protoplanetary disk can accrete substantialamounts of oxygen-rich planetesimals, leading to super-solar metallicities inthe envelope and solar or sub-solar C/O ratios. Pebble accretion has beendemonstrated to play an important role in core accretion and to have growthrates that are consistent with planetary migration. The high pebble accretionrates allow planetary cores to start their growth beyond 10 AU and subsequentlymigrate to cold (>~ 1 AU), warm (~0.1 AU- 1AU) or hot (<~ 0.1 AU) orbits. Inthis work we investigate how the formation of giant planets via pebbleaccretion influences their atmospheric chemical compositions. We find thatunder the standard pebble accretion scenario, where the core is isolated fromthe envelope, the resulting metallicities (O/H and C/H ratios) are sub-solar,while the C/O ratios are super-solar. Planets that migrate through the disk tobecome hot Jupiters accrete substantial amounts of water vapour, but stillacquire slightly sub-solar O/H and super-solar C/O of 0.7-0.8. The metallicitycan be substantially sub-solar (~0.2-0.5x solar) and the C/O can even approach1.0 if the planet accretes its envelope mostly beyond the CO2 ice line, i.e.cold Jupiters or hot Jupiters that form far out and migrate in by scattering.Allowing for core erosion yields significantly super-solar metallicities andsolar or sub-solar C/O, which can also be achieved by other means, e.g.photo-evaporation and late-stage planetesimal accretion.

Atmospheric Signatures of Giant Exoplanet Formation by Pebble Accretion