This article reviews our current understanding of terrestrial planet formation. The focus is on
computer simulations of the dynamical aspects of the accretion process. Throughout the …

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 …

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 riddle posed by super-Earths (1–4R⊕, 2–20M⊕) is that they are not Jupiters: their core
masses are large enough to trigger runaway gas accretion, yet somehow super-Earths …

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 …

Aims. We attempt to explain grain growth to mm sized particles and their retention in the
outer regions of protoplanetary disks, as observed at sub-mm and mm wavelengths, by …

The merger rate of stellar-mass black hole binaries (sBHBs) inferred by the Advanced Laser
Interferometer Gravitational-Wave Observatory (LIGO) suggests the need for an efficient …

How big were the first planetesimals? We attempt to answer this question by conducting
coagulation simulations in which the planetesimals grow by mutual collisions and form …

Earth's global magnetic field arises from vigorous convection within the liquid outer core.
Palaeomagnetic evidence reveals that the geodynamo has operated for at least 3.4 billion …

Planetary embryos embedded in gaseous protoplanetary disks undergo Type I orbital
migration. Migration can be inward or outward depending on the local disk properties but, in …