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A low mass for Mars from Jupiter’s early gas-driven migration
Simulation of the early Solar System shows how the inward migration of Jupiter to 1.5 au, and its subsequent outward migration, lead to a planetesimal disk truncated at 1’au; the terrestrial planets then form from this disk over the next 30–50 million years, with an Earth/Mars mass ratio consistent with observations. Expand
Prior work has found that a variety of terrestrial planetary compositions are expected to occur within known extrasolar planetary systems. However, such studies ignored the effects of giant planetExpand
Building the terrestrial planets: Constrained accretion in the inner Solar System
Abstract To date, no accretion model has succeeded in reproducing all observed constraints in the inner Solar System. These constraints include: (1) the orbits, in particular the smallExpand
Iron meteorites as remnants of planetesimals formed in the terrestrial planet region
It is shown that the iron-meteorite parent bodies most probably formed in the terrestrial planet region, and it is predicted that some asteroids are main-belt interlopers and a select few may even be remnants of the long-lost precursor material that formed the Earth. Expand
Terrestrial planet formation with strong dynamical friction
Abstract We have performed 8 numerical simulations of the final stages of accretion of the terrestrial planets, each starting with over 5× more gravitationally interacting bodies than in any previousExpand
Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water
Abstract In order to test accretion simulations as well as planetary differentiation scenarios, we have integrated a multistage core–mantle differentiation model with N-body accretion simulations.Expand
Highly siderophile elements in Earth’s mantle as a clock for the Moon-forming impact
A large number of N-body simulations are used to demonstrate a relationship between the time of the last giant impact on an Earth-like planet and the amount of mass subsequently added during the era known as Late Accretion, and the concentration of highly siderophile elements in Earth’s mantle constrains the mass of chondritic material added to Earth during LateAccretion. Expand
The collisional and dynamical evolution of the main-belt and NEA size distributions
Abstract The size distribution of main belt of asteroids is determined primarily by collisional processes. Large asteroids break up and form smaller asteroids in a collisional cascade, with theExpand
The global effects of impact-induced seismic activity on fractured asteroid surface morphology
Abstract Impact-induced seismic vibrations have long been suspected of being an important surface modification process on small satellites and asteroids. In this study, we use a series of linkedExpand
Making the Earth: Combining Dynamics and Chemistry in the Solar System
Abstract No terrestrial planet formation simulation completed to date has considered the detailed chemical composition of the planets produced. While many have considered possible water contents andExpand