Introduction
Sub‑Neptune planets, sized between Earth and Neptune, constitute the majority of known exoplanets. Their prevalence contrasts with the limited knowledge of their bulk composition, as direct probing of their interiors remains out of reach.
Impact of Cloud Layers
Recent modeling indicates that dense cloud decks in the upper atmospheres significantly affect heat transport and internal pressure. These processes can skew mass‑radius interpretations by altering the balance between rocky material and light gases.
Potential Interior Scenarios
Depending on cloud chemistry, a sub‑Neptune may host a solid core shrouded by a thick hydrogen‑helium envelope, or it could be dominated by volatiles such as water, ammonia, or carbon‑bearing molecules. The study suggests a strong link between cloud formation and the presence of such volatiles.
Implications for Future Observations
The findings highlight the need to incorporate cloud physics into the analysis of transit and radial‑velocity data. Upcoming infrared spectroscopy missions will be better equipped to detect signatures that reveal the true interior makeup of these worlds.