Constraining the volatile fraction of planets from transit observations

TL;DR

This paper presents a method to infer the volatile content of transiting exoplanets using planetary structure models and observations, helping to understand planet formation and composition.

Contribution

It introduces a novel approach to constrain planetary volatile fractions from transit data, especially considering evaporation effects and evolutionary ages.

Findings

At least 20% volatiles in 55 Cnc e assuming no gas envelope.

Method can constrain volatile content for close-in planets with evaporated atmospheres.

Statistical constraints on volatile fractions for planets at different ages.

Abstract

The determination of the abundance of volatiles in extrasolar planets is very important as it can provide constraints on transport in protoplanetary disks and on the formation location of planets. However, constraining the internal structure of low-mass planets from transit measurements is known to be a degenerate problem. Using planetary structure and evolution models, we show how observations of transiting planets can be used to constrain their internal composition, in particular the amount of volatiles in the planetary interior, and consequently the amount of gas (defined in this paper to be only H and He) that the planet harbors. We show for low-mass gas-poor planets that are located close to their central star that assuming evaporation has efficiently removed the entire gas envelope, it is possible to constrain the volatile fraction of close-in transiting planets. We illustrate this method on the example of 55 Cnc e and show that under the assumption of the absence of gas, the measured mass and radius imply at least 20 % of volatiles in the interior. For planets at larger distances, we show that the observation of transiting planets at different evolutionary ages can be used to set statistical constraints on the volatile content of planets. These results can be used in the context of future missions like PLATO to better understand the internal composition of planets.