Atmospheres of Rocky Exoplanets

TL;DR

This paper reviews recent advances in understanding rocky exoplanet atmospheres, highlighting their diversity, evolution, and the potential for biosignature detection with upcoming observational capabilities.

Contribution

It provides a comprehensive overview of theoretical progress, observational constraints, and future directions in characterizing rocky exoplanet atmospheres.

Findings

Many rocky planets may initially have hydrogen-helium envelopes.

Diverse atmospheric compositions are expected due to various factors.

Observations have ruled out hydrogen atmospheres on some nearby rocky exoplanets.

Abstract

Rocky planets are common around other stars, but their atmospheric properties remain largely unconstrained. Thanks to a wealth of recent planet discoveries and upcoming advances in observing capability, we are poised to characterize the atmospheres of dozens of rocky exoplanets in this decade. Theoretical understanding of rocky exoplanet atmospheres has advanced considerably in the last few years, yielding testable predictions of their evolution, chemistry, dynamics and even possible biosignatures. Here we review key progress in this field to date and discuss future objectives. Our major conclusions are as follows: 1) Many rocky planets may form with initial H$_2$-He envelopes that are later lost to space, likely due to a combination of stellar UV/X-ray irradiation and internal heating. 2) After the early stages of evolution, a wide diversity of atmospheric compositions is expected, due to variations in host star flux, atmospheric escape rates, interior exchange and other factors. 3) Observations have ruled out the presence of hydrogen-dominated atmospheres on several nearby rocky exoplanets, and the presence of any thick atmosphere on one target. More detailed atmospheric characterization of these planets and others will become possible in the near future. 4) Exoplanet biosphere searches are an exciting future goal. However, reliable detections for a representative sample of planets will require further advances in observing capability and improvements in our understanding of abiotic planetary processes.