Photochemical Haze Formation in the Atmospheres of super-Earths and mini-Neptunes

TL;DR

This study investigates how UV-driven photochemical haze particles form in super-Earth and mini-Neptune atmospheres with varying metallicities and temperatures, providing insights into exoplanet atmospheric processes.

Contribution

It introduces UV photochemistry experiments to simulate haze formation in high-metallicity exoplanet atmospheres, expanding understanding beyond previous plasma-based studies.

Findings

Haze particles form across all metallicities and temperatures.

Particle size decreases with increasing temperature.

Haze production rates are temperature-dependent.

Abstract

UV radiation can induce photochemical processes in exoplanet atmospheres and produce haze particles. Recent observations suggest that haze and/or cloud layers could be present in the upper atmospheres of exoplanets. Haze particles play an important role in planetary atmospheres and may provide a source of organic material to the surface which may impact the origin or evolution of life. However, very little information is known about photochemical processes in cool, high-metallicity exoplanetary atmospheres. Previously, we investigated haze formation and particle size distribution in laboratory atmosphere simulation experiments using AC plasma as the energy source. Here, we use UV photons to initiate the chemistry rather than the AC plasma, since photochemistry driven by UV radiation is important for understanding exoplanet atmospheres. We present photochemical haze formation in current UV experiments, we investigated a range of atmospheric metallicities (100x, 1000x, and 10000x solar metallicity) at three temperatures (300 K, 400 K, and 600 K). We find that photochemical hazes are generated in all simulated atmospheres with temperature-dependent production rates: the particles produced in each metallicity group decrease as the temperature increases. The images taken with atomic force microscopy show the particle size (15-190 nm) varies with temperature and metallicity. Our laboratory experimental results provide new insight into the formation and properties of photochemical haze, which could guide exoplanet atmosphere modeling and help to analyze and interpret current and future observations of exoplanets.