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Super-Earths and mini-Neptunes are the most abundant types of planets amongthe ~3500 confirmed exoplanets, and are expected to exhibit a wide variety ofatmospheric compositions. Recent transmission spectra of super-Earths andmini-Neptunes have demonstrated the possibility that exoplanets have haze/cloudlayers at high altitudes in their atmospheres. However, the compositions, sizedistributions, and optical properties of these particles in exoplanetatmospheres are poorly understood. Here, we present the results of experimentallaboratory investigations of photochemical haze formation within a range ofplanetary atmospheric conditions, as well as observations of the color and sizeof produced haze particles. We find that atmospheric temperature andmetallicity strongly affect particle color and size, thus altering theparticles' optical properties (e.g., absorptivity, scattering, etc.); on alarger scale, this affects the atmospheric and surface temperature of theexoplanets, and their potential habitability. Our results provide constraintson haze formation and particle properties that can serve as critical inputs forexoplanet atmosphere modeling, and guide future observations of super-Earthsand mini-Neptunes with the Transiting Exoplanet Survey Satellite (TESS), theJames Webb Space Telescope (JWST), and the Wide-Field Infrared Survey Telescope(WFIRST).

Laboratory Simulations of Haze Formation in the Atmospheres of super-Earths and mini-Neptunes: Particle Color and Size Distribution