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Making the Moon from a Fast-Spinning Earth: A Giant Impact Followed by Resonant Despinning
Forming the Moon from Earth It is thought that the Moon formed after a Mars-sized planet hit Earth about 4.5 billion years ago. Computer simulations of this event predict that the Moon was producedExpand
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Velocity-Dependent Catastrophic Disruption Criteria for Planetesimals
The resistance of planetesimals to collisional erosion changes dramatically during planet formation. The transition between accretion and erosion from a collision is defined by the relationshipExpand
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COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS
Collisions are the core agent of planet formation. In this work, we derive an analytic description of the dynamical outcome for any collision between gravity-dominated bodies. We conductExpand
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Full numerical simulations of catastrophic small body collisions
Abstract The outcome of collisions between small icy bodies, such as Kuiper belt objects, is poorly understood and yet a critical component of the evolution of the trans-neptunian region. TheExpand
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Records of an ancient Martian magnetic field in ALH84001
Although Mars does not presently appear to have a global dynamo magnetic field, strong crustal fields have recently been detected by the Mars Global Surveyor above surfaces formed ∼3 or more Ga. WeExpand
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Collisional Stripping and Disruption of Super-Earths
The final stage of planet formation is dominated by collisions between planetary embryos. The dynamics of this stage determine the orbital configuration and the mass and composition of planets in theExpand
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The Formation of the Collisional Family Around the Dwarf Planet Haumea
Haumea, a rapidly rotating elongated dwarf planet ({approx}1500 km in diameter), has two satellites and is associated with a 'family' of several smaller Kuiper Belt objects (KBOs) in similar orbits.Expand
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Evolution and persistence of 5‐μm hot spots at the Galileo probe entry latitude
We present a study on the longitudinal locations, morphology, and evolution of the 5-μm hot spots at 6.5°N latitude (planetocentric) from an extensive Infrared Telescope Facility-National ScienceExpand
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COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION
Numerical simulations of the stochastic end stage of planet formation typically begin with a population of embryos and planetesimals that grow into planets by merging. We analyzed the impactExpand
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Martian subsurface properties and crater formation processes inferred from fresh impact crater geometries
The geometry of simple impact craters reflects the properties of the target materials, and the diverse range of fluidized morphologies observed in Martian ejecta blankets are controlled by theExpand
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