The disks that orbit young stars are the essential conduits and reservoirs of material for star
and planet formation. Their structures, meaning the spatial variations of the disk physical …

The solid content of circumstellar disks is inherited from the interstellar medium: dust
particles of at most a micrometer in size. Protoplanetary disks are the environment where …

Abstract 'Hot super-Earths'(or 'mini-Neptunes') between one and four times Earth's size with
period shorter than 100 d orbit 30–50 per cent of Sun-like stars. Their orbital configuration …

The growth of a planetary core by pebble accretion stops at the so-called pebble isolation
mass, when the core generates a pressure bump that traps drifting pebbles outside its orbit …

Turbulence is a fundamental parameter in models of grain growth during the early stages of
planet formation. As such, observational constraints on its magnitude are crucial. Here we …

Turbulence can transport angular momentum in protoplanetary disks and influence the
growth and evolution of planets. With spatially and spectrally resolved molecular emission …

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 …

We analyse the stability and non-linear dynamics of power-law accretion disc models. These
have mid-plane densities that follow radial power laws and have either temperature or …

Accumulation of dust and ice particles into planetesimals is an important step in the planet
formation process. Planetesimals are the seeds of both terrestrial planets and the solid cores …

The formation of planets with gaseous envelopes takes place in protoplanetary accretion
discs on time scales of several million years. Small dust particles stick to each other to form …