Discs of gas and dust around million-year-old stars are a by-product of the star formation
process and provide the raw material to form planets. Hence, their evolution and dispersal …

The Juno mission has revolutionized and challenged our understanding of Jupiter. As Juno
transitioned into its extended mission, we review the major findings of Jupiter's internal …

In the solar system giant planets come in two flavours: gas giants (Jupiter and Saturn) with
massive gas envelopes, and ice giants (Uranus and Neptune) with much thinner envelopes …

The formation of planets depends on the underlying protoplanetary disc structure, which in
turn influences both the accretion and migration rates of embedded planets. The disc itself …

The formation of planetary cores must proceed rapidly in order for the giant planets to
accrete their gaseous envelopes before the dissipation of the protoplanetary gas disc (≲ 3 …

Close-in super-Earths having radii 1–4 R⊕ may possess hydrogen atmospheres comprising
a few percent by mass of their rocky cores. We determine the conditions under which such …

Chemical compositions of giant planets provide a means to constrain how and where they
form. Traditionally, super-stellar elemental abundances in giant planets were thought to be …

Context. Observations have revealed in the Kepler data a depleted region separating
smaller super-Earths from larger sub-Neptunes. This can be explained as an evaporation …

Motivated by recent spectroscopic evidence for carbon-rich atmospheres on some transiting
exoplanets, we investigate the influence of the C/O ratio on the chemistry, composition, and …

Protoplanetary disks are the sites of planet formation, and the evolution and eventual
dispersal of these disks strongly influences the formation of planetary systems. Disk …