Simulations of a late lunar-forming impact

By R. Canup. 2004

598 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/bc0e98bbd47f1a9144bcbbb90e2996331e4df689

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In Astronomy and Astrophysics

Citations in the corpus

Turbulent Mixing of Metal and Silicate during Planet Accretion – and interpretation of the Hf-W chronometer (2010, background): “Simulations give the impression of some “mixing” in the sense that particles of iron and silicate can become intermingled (Canup, 2004).”
THE Hf-W ISOTOPIC SYSTEM AND THE ORIGIN OF THE EARTH AND MOON (2005, background): “However, as discussed earlier, from the recent higher resolution SPH work of Canup (2004), it appears that differentiation following a Mars-sized giant impactor will follow the general model discussed here (impactor metal reequilibrated in the magma ocean) and not a core-penetrative mode.”
Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, methodology): “However, we note that the simulations of Canup (2004, 2008) were specifically designed to reproduce the details of the Earth-Moon system, in particular its high specific angular momentum and the Moon’s small core.”
Accretion of Saturn's mid-sized moons during the viscous spreading of young massive rings: Solving the paradox of silicate-poor rings versus silicate-rich moons (2011, background): “…be preferentially disrupted (because of shock-wave reflection at the core/mantle boundary) and scattered into orbit (as was the case for the proto-Earth during the impact that resulted in the formation of the Earth’s Moon; see e.g., Canup, 2004) and might result in the formation of an icy ring.”
Thermal evolution of the Earth: Secular changes and fluctuations of plate characteristics (2007, background): “This impact was energetic enough to melt the entire planet [e.g. (Canup, 2004)].”
Emergence of a Habitable Planet (2007, background): “The apparent success of the Moon-forming impact hypothesis (Benz et al. 1986; Hartmann et al. 1986; Stevenson 1987; Canup and Righter 2000; Canup and Asphaug 2001; Canup 2004) has probably evaporated any lingering doubts.”
Planetary and meteoritic Mg/Si and δ30Si variations inherited from solar nebula chemistry (2015, background): “, 2014a), which was difficult to explain in the context of silicon isotopic fractionation during core formation as in most giant impact scenarios, most of the Moon is thought to have come from the impactor (Canup, 2004; however see Ćuk and Stewart 2012; Canup 2012) and Earth-Moon equilibration scena”
Accretion Efficiency during Planetary Collisions (2004, background): “5–0.9M 0.1–0.3M with (see, e.g., Benz et al. 1989; Cameronv p 1.0v –1.2vimp esc esc 2001; Canup & Asphaug 2001; Canup 2004).”
Formation of Phobos and Deimos via a giant impact (2015, methodology): “…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).”
COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. II. THE DIVERSITY OF IMPACT OUTCOMES DURING THE END STAGE OF PLANET FORMATION (2011, methodology): “The formation of Earth’s Moon (Canup 2004), the Pluto system (Canup 2005), and the Haumea system (Leinhardt et al. 2010) 2 These data are derived from Table 1 in Leinhardt et al. (2000).”
Detailed Models of Super-Earths: How Well Can We Infer Bulk Properties? (2007, background): “Conversely, any process that targets heavy elements to be excluded from accretion ( like formation of the Moon after the Mars-sized impact onto a proto-Earth; Canup 2004) would deplete the planet from Fe and silicates forming a light planet (mantle, mantle+water ocean planets).”