Exoplanet habitability research advances

Early July 2026 JWST data showed that vapor‑rock and salt clouds on sub‑Neptune planets can trap heat, raising temperatures at the atmosphere‑interior boundary by more than 1,000 °C and potentially driving global magma oceans that release gases such as oxygen and silicon compounds. Days later a University of Pennsylvania‑Japan team modeled the tidally‑locked rocky world LHS 3844b, finding a stable mantle circulation that transports heat from a blistering day side (1,000‑2,000 K) to an icy night side, creating twilight zones, stationary mantle plumes and a possible magnetic field. Mid‑July laboratory analogues reproduced the extreme temperature contrast, confirming the “planetary pulse” circulation and suggesting moderate‑temperature niches on such worlds. Separate work on the habitable‑zone super‑Earth LHS 1140 b detected helium escaping from a high‑altitude atmosphere with the WINERED spectrograph on the Magellan Clay telescope; follow‑up observations in 2025 showed the signal weakening, indicating variable atmospheric loss. In July 2026 the Harvard‑led team refined these findings, confirming a helium‑rich upper atmosphere, quantifying its variability, and publishing the result in *Science* as the first direct confirmation of an atmosphere on a rocky exoplanet inside its star’s Goldilocks zone. The detection underscores LHS 1140 b’s potential to retain a water‑rich envelope, its suitability for biosignature searches, and its priority for forthcoming James Webb observations.