Early Accretion of Large Amounts of Solids for Directly-Imaged Exoplanets

TL;DR

This study analyzes seven directly-imaged exoplanets and finds they accrete large amounts of solids early in their formation, enriching their atmospheres regardless of their formation mechanism.

Contribution

It provides the first population-level analysis showing that wide-separation planetary mass objects accrete significant solids early on, using a Bayesian framework with atmospheric metallicity data.

Findings

PMOs accrete over 50 Earth masses of solids on average

Individual planets accrete between 23.3 and 223.2 Earth masses of solids

Solid accretion occurs early, within approximately 2 million years

Abstract

As the number of planetary mass objects (PMOs, $\lessapprox$13 M$_{\rm{Jupiter}}$) at wider separation ($\gtrapprox$10 AU) grows, there is emerging evidence that they form differently from their higher-mass brown-dwarf (BD) counterparts. Specifically, PMOs' atmospheres are often enriched by metals and show a large dispersion of metallicity, which is usually interpreted as a sign of solid accretion. {{As a first step toward a population-level study of the amount and timing of solid accretion, }}we analyze a sample of seven directly-imaged exoplanets with measured stellar and planetary chemical abundances (51 Eri b, $\beta$ Pic b, HIP 65426 b, HR 8799 c and e, AF Lep b, and YSES 1 c). Our analysis uses existing data of stellar and planetary atmospheric metallicities, and adopts a Bayesian framework that marginalizes the probabilities of disk conditions, formation locations, {{planetary interior structures}}, and accretion physics. We show that these PMOs accrete large amounts of solids {{regardless of whether they form via core accretion or disk instability}}. On average $\gtrapprox$50 M$_\oplus$ solids are accreted to enrich planet atmospheres. {{Individual planet accretes between 23.3 and 223.2 M$_\oplus$ of solid mass, more than 75\% of which is assumed to stay in the atmosphere and increase the observed metallicity.}} The result implies that the solid accretion process and therefore the planet formation process {{likely take place}} at an early stage {{($\lessapprox$2 Myr)}} when large amounts of solids are available in young {{massive}} protoplanetary disks.