The moniker rubble pile is typically applied to all Solar System bodies> 200 m and<∼ 10 km
in diameter; in this size range, there is an abundance of evidence that nearly every object is …

Planets are expected to conclude their growth through a series of giant impacts: energetic,
global events that significantly alter planetary composition and evolution. Computer models …

We present numerical simulations of terrestrial planet formation that examine the growth
continuously from planetesimals to planets in the inner Solar System. Previous studies show …

Chondrules, mm-sized igneous-textured spherules, are the dominant bulk silicate
constituent of chondritic meteorites and originate from highly energetic, local processes …

Terrestrial planet formation theory is at a bottleneck, with the growing realization that
pairwise collisions are treated far too simply. Here, and in our companion paper that …

In the canonical model of Moon formation, a Mars-sized protoplanet" Theia" collides with
proto-Earth at close to their mutual escape velocity v esc and a common impact angle∼ 45 …

The absence of planets interior to Mercury continues to puzzle terrestrial-planet formation
models, particularly when contrasted with the relatively high derived occurrence rates of …

Using smoothed particle hydrodynamics we model giant impacts of Super-Earth mass rocky
planets between an atmosphere-less projectile and an atmosphere-rich target. In this work …

Collisions between large, similar-sized bodies are believed to shape the final characteristics
and composition of terrestrial planets. Their inventories of volatiles such as water are either …

We develop empirical relationships for the accretion and erosion of colliding gravity-
dominated bodies of various compositions under conditions expected in late-stage solar …