Planetary Albedo Is Limited by the Above-cloud Atmosphere: Implications for Sub-Neptune Climates

Abstract

Energy limits that delineate the “habitable zone” for exoplanets depend on a given exoplanet’s net planetary albedo (or “Bond albedo”). We here demonstrate that the planetary albedo of an observed exoplanet is limited by the above-cloud atmosphere—the region of the atmosphere that is probed in remote observation. We derive an analytic model to explore how the maximum planetary albedo depends on the above-cloud optical depth and scattering versus absorbing properties, even in the limit of a perfectly reflective gray cloud layer. We apply this framework to sub-Neptune K2-18b, for which a high planetary albedo has recently been invoked to argue for the possibility of maintaining a liquid-water ocean surface, despite K2-18b receiving an energy flux from its host star that places it inside of its estimated “habitable zone” inner edge. We use a numerical multiple-scattering line-by-line radiative transfer model to retrieve the albedo of K2-18b based on the observational constraints from the above-cloud atmosphere. Our results demonstrate that K2-18b’s observed transmission spectrum already restricts its possible planetary albedo to values below the threshold required to be potentially habitable, with the data favoring a median planetary albedo of 0.17–0.18. Our results thus reveal that currently characterizable sub-Neptunes are likely to be magma-ocean or gas-dwarf worlds. The methods that we present are generally applicable to constrain the planetary albedo of any exoplanet with measurements of its observable atmosphere, enabling the quantification of potential exoplanet habitability with current observational capabilities.