Planets, embedded in their natal discs, harbour hot envelopes. When pebbles are accreted
by these planets, the contained volatile components may sublimate, enriching the envelope …

Abstract Planets with 2 R⊕< R< 3 R⊕ and orbital period< 100 days are abundant; these
sub-Neptune exoplanets are not well understood. For example, Kepler sub-Neptunes are …

During their formation, planets form large, hot atmospheres due to the ongoing accretion of
solids. It has been customary to assume that all solids end up at the center, constituting a …

We obtained spectra of the pre-main-sequence star AU Microscopii during a transit of its
Neptune-sized planet to investigate its orbit and atmosphere. We used the high-dispersion …

Mildly irradiated mini-Neptunes have densities potentially consistent with them hosting
substantial liquid-water oceans (" Hycean" planets). The presence of CO 2 and …

The composition of the protoplanetary disc is thought to be linked to the composition of the
host star, where a higher overall metallicity provides the building blocks for planets …

Recent work suggests that many short-period super-Earth and sub-Neptune planets may
have significant spin axis tilts (" obliquities"). When planets are locked in high-obliquity …

The atmospheres of small, close-in exoplanets are vulnerable to rapid mass loss during
protoplanetary disc dispersal via a process referred to as 'boil-off', in which confining …

The low luminosity of Uranus is a long-standing challenge in planetary science. Simple
adiabatic models are inconsistent with the measured luminosity, which indicates that Uranus …

Recent observations of rocky super-Earths have revealed an apparent wider distribution of
Fe/Mg ratios, or core to mantle ratios, than the planets in our Solar system. This study aims to …