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Abstract Understanding the planetary envelope composition of sub-Neptune-type exoplanets is challenging due to the inherent degeneracy in their interior composition scenarios. Particularly, the planetary envelope’s H 2 O/H 2 ratio, which can also be expressed as the O/H ratio, provides crucial insights into its original location relative to the ice line during planetary formation. Using self-consistent radiative transfer modeling and a rate-based automatic chemical network generator combined with 1D photochemical kinetic-transport atmospheric modeling, we investigate various atmospheric scenarios of temperate sub-Neptunes, ranging from H 2 -dominated to H 2 O-dominated atmospheres with equilibrium temperatures ( T eq ) of 250—400 K. This study includes examples such as K2-18 b ( T eq = 255 K), LP 791-18 c ( T eq = 324 K), and TOI-270 d ( T eq = 354 K). Our models indicate that the atmospheric CO 2 /CH 4 ratio can be used to infer the deep interior H 2 O/H 2 ratio. Applying this method to recent JWST observations, our findings suggest that K2-18 b likely has an interior that is 50% highly enriched in water, exceeding the water content in a 100 × Z ⊙ scenario and suggesting a planetary formation mechanism involving substantial accretion of ices. In contrast, our model suggests that approximately 25% of TOI-270 d’s interior is composed of H 2 O, which aligns with the conventional metallicity framework with a metallicity higher than 100 × Z ⊙ . Furthermore, our models identify carbonyl sulfide (OCS) and sulfur dioxide (SO 2 ) as strong indicators for temperate sub-Neptunes with at least 10% of their interior composed of water. These results provide a method to delineate the internal composition and formation mechanisms of temperate sub-Neptunes ( T eq < ∼ 500 K) via atmospheric characterization through transmission spectroscopy.
Yang et al. (Thu,) studied this question.