Terrestrial planet formation with strong dynamical friction

By D. O'Brien, A. Morbidelli, Harold Levison. 2006

392 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/29866545bef89d4fdb13093716371d6634c145f2

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In Astronomy and Astrophysics

Citations in the corpus

Iapetus’ geophysics : rotation rate, shape, and equatorial ridge (2007, background): “A somewhat weaker constraint on giant planet formation time scales comes from dynamical calculations that show the presence of Jupiter and Saturn to be important determinants of the final architecture of the terrestrial planet orbits and masses (O’Brien et al., 2006), coupled with the fact that much”
The Compositional Structure of the Asteroid Belt (2015, background): “The inclination distribution is also a problem for models that invoke stranded planetary embryos that excite and deplete the primordial Asteroid Belt (see O’Brien et al., 2006).”
Heterogeneous accretion, composition and core–mantle differentiation of the Earth (2011, background): “Accretion models show that late accreting bodies, on average, come from larger heliocentric distances (Bond et al., 2010; O'Brien et al., 2006).”
Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water (2014, background): “100 km in diameter (O’Brien et al., 2006).”
Origins of volatile elements (H, C, N, noble gases) on Earth and Mars in light of recent results from the ROSETTA cometary mission (2016, positive): “…suggest that, during its formation, the Earth accreted water and other volatile elements predominantly from planetesimals parented to primitive asteroids, i.e. with composition similar to carbonaceous chondrites (Morbidelli et al., 2000; Raymond et al., 2004, 2007; O’Brien et al., 2006, 2014).”
Linked magma ocean solidification and atmospheric growth for Earth and Mars (2008, background): “therein) or volatile-rich material from greater radii in the planetary disk may have been added later in planetary formation (e.g., Raymond et al., 2006; O'Brien et al., 2006).”
Water delivery and giant impacts in the 'Grand Tack' scenario (2014, positive): “In comparison, the median value of t imp in the simulations of O’Brien et al. (2006) with a dynamically cold Jupiter is (cid:2) 75 Myr.”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “The classical model (Wetherill, 1996; Chambers and Wetherill, 1998; Chambers, 2001; Levison and Agnor, 2003; O’Brien et al., 2006; Raymond et al., 2006, 2009, 2014; Morishima et al., 2008, 2010; Fischer et al., 2014) proposes that the giant planets formed near their current locations and influenced…”