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 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 …

Rapid orbital drift of macroscopic dust particles is one of the major obstacles to planetesimal
formation in protoplanetary disks. We re-examine this problem by considering the porosity …

Collisions are the core agent of planet formation. In this work, we derive an analytic
description of the dynamical outcome for any collision between gravity-dominated bodies …

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 …

Several exoplanets have recently been imaged at wide separations of> 10 AU from their
parent stars. These span a limited range of ages (< 50 Myr) and atmospheric properties, with …

Pebble accretion is the mechanism in which small particles (“pebbles”) accrete onto big
bodies (planetesimals or planetary embryos) in gas-rich environments. In pebble accretion …

Gas-giant planets, such as Jupiter, Saturn, and massive exoplanets, were formed via the gas
accretion onto the solid cores, each with a mass of roughly 10 Earth masses. However, rapid …

The radii of debris disks and the sizes of their dust grains are important tracers of the
planetesimal formation mechanisms and physical processes operating in these systems …

Secular gravitational instability (GI) is one promising mechanism for creating annular
substructures and planetesimals in protoplanetary disks. We perform numerical simulations …