Planets form in disks of gas and dust around young stars. The disk molecular reservoirs and
their chemical evolution affect all aspects of planet formation, from the coagulation of dust …

The detection and characterization of large populations of pebbles in protoplanetary disks
have motivated the study of pebble accretion as a driver of planetary growth. This review …

The formation of planetesimals is expected to occur via particle-gas instabilities that
concentrate dust into self-gravitating clumps,–. Triggering these instabilities requires the …

The streaming instability (SI) is a mechanism to aerodynamically concentrate solids in
protoplanetary disks and trigger the formation of planetesimals. The SI produces strong …

The observed lifetimes of gaseous protoplanetary discs place strong constraints on gas and
ice giant formation in the core accretion scenario. The approximately 10-Earth-mass solid …

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 …

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 …

Close-in super-Earths, with radii R≈ 2–5 R⊕ and orbital periods P< 100 d, orbit more than
half, and perhaps nearly all, Sun-like stars in the Universe. We use this omnipresent …

Protoplanetary disks are quasi-steady structures whose evolution and dispersal determine
the environment for planet formation. I review the theory of protoplanetary disk evolution and …

Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical
units are found around almost all low-mass stars shortly after their birth. These disks …