The planetary building blocks that formed in the terrestrial planet region were likely very dry,
yet water is comparatively abundant on Earth. Here we review the various mechanisms …

Our understanding of planet formation has been rapidly evolving in recent years. The
classical planet formation theory, developed when the only known planetary system was our …

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 …

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 …

Abstract Models of planet formation are built on underlying physical processes. In order to
make sense of the origin of the planets we must first understand the origin of their building …

A snow-line is the region of a protoplanetary disk at which a major volatile, such as water or
carbon monoxide, reaches its condensation temperature. Snow-lines play a crucial role in …

At least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii
and orbital periods of less than 100 days. We use N-body simulations including a model for …

Aims. We investigate the evolution of protoplanetary discs (PPDs) with magnetically driven
disc winds and viscous heating. Methods. We considered an initially massive disc with~ 0.1 …

The terrestrial planets and the asteroids dominant in the inner asteroid belt are water poor.
However, in the protoplanetary disk the temperature should have decreased below water …

Atmospheric chemical abundances of giant planets lead to important constraints on
planetary formation and migration. Studies have shown that giant planets that migrate …