The isotopic dichotomy between non-carbonaceous (NC) and carbonaceous (CC)
meteorites indicates that meteorite parent bodies derive from two genetically distinct …

Geochemical and astronomical evidence demonstrates that planet formation occurred in two
spatially and temporally separated reservoirs. The origin of this dichotomy is unknown. We …

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 …

Meteorites, and in particular primitive meteorites (chondrites), are irreplaceable probes of
the solar protoplanetary disk. We review their essential properties and endeavour to place …

Dust growth is often neglected when building models of protoplanetary disks due to its
complexity and computational expense. However, it does play a major role in shaping the …

Dust growth and its associated dynamics play key roles in the first phase of planet formation
in young stellar objects. Observations have detected signs of dust growth in very young …

Two fundamentally different processes of rocky planet formation exist, but it is unclear which
one built the terrestrial planets of the solar system. They formed either by collisions among …

In the pebble accretion scenario, the pebbles that form planets drift inward from the outer
disk regions, carrying water ice with them. At the water ice line, the water ice on the inward …

Recent analyses have shown that the concluding stages of giant planet formation are
accompanied by the development of a large-scale meridional flow of gas inside the …

Nucleosynthetic isotope variations are powerful tools to investigate genetic relationships
between meteorite groups and planets. They are instrumental to assess the early evolution …