Theory and observations point to the occurrence of magma ponds or oceans in the early
evolution of terrestrial planets and in many early-accreting planetesimals. The apparent …

An accurate assessment of the bulk chemical composition of Mars is fundamental to
understanding planetary accretion, differentiation, mantle evolution, the nature of the …

The Lutetium–Hafnium radiogenic isotopic system is widely used as a chronometer and
tracer of planetary evolution. In order for this isotopic system to fulfill its potential in planetary …

The detection of deep reflected S waves on Mars inferred a core size of 1,830±40 km (ref.),
requiring light-element contents that are incompatible with experimental petrological …

Comparing compositional models of the terrestrial planets provides insights into
physicochemical processes that produced planet-scale similarities and differences. The …

Martian meteorites are the only direct samples from Mars, thus far. Currently, there are a total
of 262 individual samples originating from at least 11 ejection events. Geochemical …

Terrestrial planets are thought to have formed through collisions between large planetary
embryos of diameter∼ 1,000–5,000 km. For Earth, the last of these collisions involved an …

The 182Hf–182W systematics of meteoritic and planetary samples provide firm constraints
on the chronology of the accretion and earliest evolution of asteroids and terrestrial planets …

We address the first several hundred million years of Earth's history. The Moon-forming
impact left Earth enveloped in a hot silicate atmosphere that cooled and condensed over∼ …

The highly siderophile elements (HSE) pose a challenge for planetary geochemistry. They
are normally strongly partitioned into metal relative to silicate. Consequently, planetary core …