The Heavy-element Content Trend of Planets: A Tracer of Their Formation Sites

Identification of the main planet formation site is fundamental to understanding how planets form and migrate to their current locations. We consider the heavy-element content trend of observed exoplanets, derived from improved measurements of mass and radius, and explore how this trend can be used as a tracer of their formation sites. Using gas accretion recipes obtained from hydrodynamical simulations, we confirm that the disk-limited gas accretion regime is most important for reproducing the trend. Given that such a regime is specified by two characteristic masses of planets, we compute these masses as a function of the distance (r) from the central star, and then examine how the regime appears in the mass–semimajor axis diagram. Our results show that a plausible solid accretion region emerges at r ≃ 0.6 au and expands with increasing r, using the conventional disk model. Given that exoplanets that possess the heavy-element content trend distribute currently near their central stars, our results imply the importance of planetary migration that would occur after solid accretion onto planets might be nearly completed at r ≥ 0.6 au. Self-consistent simulations would be needed to verify the predictions herein.