Microphysics of Water Clouds in the Atmospheres of Y Dwarfs and Temperate Giant Planets

Water clouds are expected to form on Y dwarfs and giant planets with equilibrium temperatures near or below that of Earth, drastically altering their atmospheric compositions albedos thermal emission spectra. Here we use the 1D Community Aerosol Radiation Model for Atmospheres (CARMA) investigate microphysics water cool substellar worlds constrain typical particle sizes vertical extent, taking into consideration nucleation condensation, which have not been considered in detail H/He atmospheres. We compute a small grid dwarf temperate exoplanet atmosphere models forming through homogeneous heterogeneous cloud condensation nuclei composed meteoritic dust, organic photochemical hazes, upwelled potassium chloride particles. present comparisons Ackerman & Marley parameterization physics extract optimal sedimentation efficiency parameter (f$_{sed}$) using Virga. find no Virga model replicates CARMA exactly transition f$_{sed}$ occurs from base top. Furthermore, generate simulated geometric albedo spectra large, wavelength-dependent differences between models, different gas absorption bands reacting differently distributions particularly large M band. Therefore, constraining vertically-dependent properties will be essential estimating abundances these