Dynamics of Lunar Formation

By R. Canup. 2004

254 citations recorded by the source corpus.

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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): “…and tracked for an additional 400 Myr. needed to complete the terrestrial planets are also longer than suggested by the Moon-forming impact on Earth (∼25– 30 Myr after the formation of the Solar System), which likely marked the end of significant accretion on Earth (see review by Canup, 2004).”
The naked planet Earth: Most essential pre-requisite for the origin and evolution of life (2013, background): “…been interpreted as the final residue of magma ocean when the Moonwas formed by the giant impact that led to the formation of the early Earth (e.g., Canup, 2004), where Mars-sized S.M aruyam a et al./ G eoscience Frontiers 4 (2013) 141 e 165 144 Sm 0.1471 0.406 0.239 2.755 3.21 2.733 3.52 3.11…”
Evidence for Mo isotope fractionation in the solar nebula and during planetary differentiation (2014, background): “The resulting temperature of 1800 ± 200 ◦C is in excellent agreement with other, independent estimates of core formation temperatures for the Moon.”
The faint young Sun problem (2012, background): “The prevailing theory for the formation of the Moon suggests that the Moon was created when a large (roughly Mars-sized) impactor hit the young Earth [Hartmann and Davis, 1975; Cameron and Ward , 1976; Canup, 2004], requiring the accumulation of a significant amount of material before the impact.”
“New” lunar meteorites: Implications for composition of the global lunar surface, lunar crust, and the bulk Moon (2005, background): “Detailed modeling of the impact consistently suggests that at least 75% of the lunar material comes from the late-arriving, and in a sense interloping, giant impactor (Canup 2004; cf. Benz et al. 1986; Melosh and Sonnett 1986; Canup and Asphaug 2001).”
Thermodynamics of mantle minerals - II. Phase equilibria (2011, background): “We may explore the response of the planet to a sudden increase in energy, provided, for example, by a giant impact of the type that is thought to have formed Earth’s moon (Canup 2004).”
Magma oceans in the inner solar system (2012, background): “The impactor also may be partially devolatilized upon impact (O’Keefe & Ahrens 1977, Canup 2004, Ni & Ahrens 2005, Pahlevan & Stevenson 2007); if this is the case, then retention of the atmosphere and its interaction with the magma ocean become the pertinent questions.”
The lunar magma ocean: Reconciling the solidification process with lunar petrology and geochronology (2011, background): “In the highly energetic Moon-forming giant impact of a Mars-sized body onto the proto-Earth, the system's temperature is thought to have reached 5000–10,000 K (Canup, 2004, 2008); thus any previous memory of the isotopic clock must have been reset.”
Linked magma ocean solidification and atmospheric growth for Earth and Mars (2008, background): “Second, the impactor may be devolatilized upon impact (O'Keefe and Ahrens, 1977; Canup, 2004; Ni and Ahrens, 2005; Pahlevan and Stevenson, 2007).”
Equilibration in the aftermath of the lunar-forming giant impact (2007, background): “Immediately after the giant impact, the Earth-Moon system is largely molten and partially 162 vaporized [15].”
FORMATION OF THE TERRESTRIAL PLANETS FROM A NARROW ANNULUS (2009, background): “One final point to note is that some of the late-time impactors in these simulations are considerably larger than the Mars-mass impactors traditionally used in simulations of the moon-forming impact (e.g., Canup 2004).”
Terrestrial Planet Formation. I. The Transition from Oligarchic Growth to Chaotic Growth (2005, background): “These objects are good candidates for the ‘giant impactor’ that collided with the Earth to produce the Moon (Hartmann & Davis 1975; Cameron & Ward 1976; Benz, Slattery, & Cameron 1986; Canup 2004a,b).”