Planets, embedded in their natal discs, harbour hot envelopes. When pebbles are accreted
by these planets, the contained volatile components may sublimate, enriching the envelope …

Magmatic iron-meteorite parent bodies are the earliest planetesimals in the Solar System,
and they preserve information about conditions and planet-forming processes in the solar …

Investigating the response of icy dust aggregates to water ice sublimation is essential for
understanding the formation and properties of planetesimals in protoplanetary discs …

We combine calculations of pebble accretion and accretion by large and giant impacts to
quantify the effects of pebbles on the hafnium-tungsten system during Earth formation. Our …

Water is an important component of exoplanets, with its distribution, that is, whether at the
surface or deep inside, fundamentally influencing the planetary properties. The distribution …

During protoplanetary disk formation, dust grains located in the outer disk retain their pristine
icy composition, while solids in the inner stellar-heated disk undergo volatile loss. This …

We explore the heating and differentiation of rocky planets that grow by rapid pebble
accretion. Our terrestrial planets grow outside of the ice line and initially accrete 28% water …

Whilst the formation of Solar system planets is constrained by meteoritic evidence, the
geophysical history of low-mass exoplanets is much less clear. The bulk composition and …

Rocky planets may acquire a primordial atmosphere by the outgassing of volatiles from their
magma ocean. The distribution of O between H2O, CO, and CO2 in chemical equilibrium …

Planetesimals–asteroids and comets–are the building blocks of planets in protoplanetary
discs and the source of dust, ice, and gas in debris discs. Along with planets they comprise …