Bulk and atmospheric metallicities as direct probes of sequentially varying accretion mechanisms of gas and solids onto planets

Core accretion is the standard scenario of planet formation, wherein planets are formed by sequentialaccretion of gas and solids, and is widely used to interpret exoplanet observations. However, nodirect probes of the scenario have been discussed yet. Here, we introduce an onion-like model as oneidealization of sequential accretion and propose that bulk and atmospheric metallicities of exoplanetscan be used as direct probes of the process. Our analytical calculations, coupled with observationaldata, demonstrate that the trend of observed exoplanets supports the sequential accretion hypothesis.In particular, accretion of planetesimals that are ≳ 100 km in size is most favored to consistentlyexplain the observed trends. The importance of opening gaps in both planetesimal and gas disksfollowing planetary growth is also identified. New classification is proposed, wherein most observedplanets are classified into two interior statuses: globally mixed and locally (well-)mixed. Explicitidentification of the locally (well-)mixed status enables reliable verification of sequential accretion.During the JWST era, the quality and volume of observational data will increase drastically andimprove exoplanet characterization. This work provides one key reference of how both the bulk andatmospheric metallicities can be used to constrain gas and solid accretion mechanisms of planets.