The standard model for giant planet formation is based on the accretion of solids by a
growing planetary embryo, followed by rapid gas accretion once the planet exceeds a so …

Aims. The goal of this work is to investigate Jupiter's growth by focusing on the amount of
heavy elements accreted by the planet, and to compare this with recent structure models of …

Mass-independent isotopic anomalies define two cosmochemically distinct regions: the
carbonaceous and non-carbonaceous meteorites, implying that the non-carbonaceous …

Context. The region around the H 2 O ice line, due to its higher surface density, seems to be
the ideal location to form planets. The core of Jupiter, as well as the cores of close-in gas …

Pebbles of millimeter sizes are abundant in protoplanetary discs around young stars.
Chondrules inside primitive meteorites—formed by melting of dust aggregate pebbles or in …

The evolution of protoplanetary discs embedded in stellar clusters depends on the age and
the stellar density in which they are embedded. Stellar clusters of young age and high stellar …

Observations of the population of cold Jupiter planets (r> 1 AU) show that nearly all of these
planets orbit their host star on eccentric orbits. For planets up to a few Jupiter masses …

Giant planets migrate though the protoplanetary disc as they grow their solid core and attract
their gaseous envelope. Previously, we have studied the growth and migration of an isolated …

Pebble accretion refers to the assembly of rocky planet cores from particles whose velocity
dispersions are damped by drag from circumstellar disc gas. Accretion cross-sections can …

It is widely held that the first step in forming gas-giant planets, such as Jupiter and Saturn,
was the production of solid 'cores' each with a mass roughly ten times that of the Earth …