On Modelling the Atmospheres of Potentially-Habitable Super-Earths

Abstract

Atmospheres play an important role in the habitability of a planet, so understanding and modelling them is an important step in the search for life on other planets.

This thesis presents a 1D frequency-dependent radiative-convective code that was written to help determine the temperature-pressure structure of potentially-habitable exoplanets. This code pairs with a chemistry model to determine the chemical composition of these planets' atmospheres.

This code is applied to the planets in the TRAPPIST-1 system. The initial atmospheric compositions of the TRAPPIST-1 planets are determined through planet formation history and considered for both outgassed and accreted atmospheres. An interesting result is found when running these initial atmospheric compositions through the chemistry model: when the atmosphere equilibrates, it can change its C/O ratio from equal to that found in the accreted or outgassed volatiles to something lower, because, in temperate conditions, CO$_2$ is favoured over CO. This has the consequence that observed C/O ratios in terrestrial atmospheres cannot be relied on to infer the C/O ratio of the protoplanetary disc in which the planet formed.

The initial results of atmospheric modelling for TRAPPIST-1 planets indicate that these planets are likely to have relatively warmer upper atmospheres due to the fact that their host star emits primarily in the infrared, and a portion of this radiation is then absorbed as it enters the top of the atmosphere. These initial results have not been seen in previous work.

These initial results are the beginning of a database of potential atmospheres on the TRAPPIST-1 planets. It is hoped that these atmospheres can be compared with observations from future observing missions like the James Webb Space Telescope to help constrain the surface conditions of these potentially-habitable planets and ultimately, to help in the search for life.