Accretion Efficiency during Planetary Collisions

By C. Agnor, E. Asphaug. 2004

160 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/311cd748759a316b406fdcff55dd893e031b140a

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In Astronomy and Astrophysics

Citations in the corpus

Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “Finally, CoDDEM does not track how putative effects like embryo–embryo collisions or tidal disruption between embryos and planetesimals could change the main belt's size–frequency distribution (e.g., Agnor and Asphaug, 2004; Asphaug et al., 2005).”
Terrestrial planet formation with strong dynamical friction (2006, methodology): “during large impact events (e.g., Agnor and Asphaug, 2004; Levison et al., 2005).”
Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, background): “Indeed, the majority of impacts lie in the accretionary regime as defined by Agnor & Asphaug (2004): 60%, 71%, 71%, and 75% for the four planets from the JSRES simulation (listed from closest- to farthest from the Sun), and 83%, 100% and 0% for the three EEJS planets.10 This is a larger fraction…”
Emergence of a Habitable Planet (2007, background): “Another aspect of the giant impact phase of accretion is that more than half of the collisions are bounces rather than mergers (Agnor and Asphaug 2004; Asphaug et al. 2006).”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION (2011, background): “However, hydrocode simulations of oblique collisions between embryos found that inelastic collisions, known as hit-and-run (H&R) events (Agnor & Asphaug 2004; Asphaug et al. 2006), are a common outcome at speeds just above the mu- sstewart@eps.harvard.edu zoe.leinhardt@bristol.ac.uk tual escape…”
High-resolution simulations of the final assembly of Earth-like planets I. Terrestrial accretion and dynamics (2005, unknown): “Realistic collisions between large bodies create a swarm of debris, the details of which depend on the collision velocity and angle ( Agnor & Asphaug, 2004).”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS (2011, background): “…between self-gravitating bodies of similar size have identified new types of collision outcomes including hit-and-run and mantle-stripping events (Agnor & Asphaug 2004a; Asphaug et al. 2006; Marcus et al. 2009, 2010b; Leinhardt et al. 2010; Asphaug 2010; Kokubo & Genda 2010; Benz et al. 2007;…”
Building Terrestrial Planets (2012, methodology): “Simulations of giant collisions between embryos conducted with the Smooth Particle Hydrodynamics (SPH) technique (Agnor & Asphaug 2004, Asphaug et al. 2006) show that perfect merging is rare.”
Formation of Phobos and Deimos via a giant impact (2015, background): “…used to model several types of giant impacts, including the putative Moon-forming impact (Benz et al. 1989, 1986, 1987; Cameron 1997; Cameron and Benz 1991; Canup 2004, 2008; Canup and Asphaug 2001) and other types of large-scale planetary collisions (Agnor and Asphaug 2004; Genda et al. 2012).”
Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water (2014, background): “(a) Giant hit-and-run impacts and other debris-generating impacts can occur in the protoplanetary disk (Agnor and Asphaug, 2004).”
The Evaporation Valley in the Kepler Planets (2017, background): “Giant impacts among short period planets will happen at speeds well above their surface escape velocities (Agnor & Asphaug 2004; Marcus et al. 2009), and will therefore disperse much of the original planetary envelopes.”
Chondrule formation during planetesimal accretion (2011, background): “But in fact partial accretion (ξb1) and hit and run (ξ~0) account for most collisions when φ~1 (Agnor and Asphaug, 2004).”