In situ enrichment in heavy elements of hot Jupiters

Context. Radius and mass measurements of short-period giant planets reveal that many these contain a large amount heavy elements. Although the range inferred metallicities is broad, with more than 100 M ⊕ elements are not rare. This in sharp contrast expectations conventional core-accretion model for origin planets. Aims. The proposed explanations heavy-element enrichment fall short explaining most enriched We look additional processes can explain full envelope enrichments. Methods. revisited dynamics pebbles dust vicinity using analytic estimates published results on profile gap opened by planet, radial velocity gas respect to Stokes number particles different parts disk, consequent dust/gas ratio. our derived framework viscous α -disk, we also discuss case disks driven angular momentum removal magnetized winds. Results. When far from star, confined pressure bump at outer edge planet-induced gap. reach inner part disk ( r p ≪ 2 au), instead penetrates into together gas. ratio be enhanced an order magnitude if drift impeded farther out other barriers. Thus, hot undergoing runaway accretion swallow dust, acquiring ~100 time they Jupiter masses. Conclusions. Whereas accreted very dust-poor, extremely dust-rich. provided fraction atmosphere Jupiters situ, as well. draw distinction between this process pebble (i.e., capture without gas), which ineffective small stellocentric radii, even super-Earths. Giant effective barriers against flow across their Saturn Jupiter, after locking mutual mean motion resonance reversing migration, could have debris.