The Primordial Excitation and Clearing of the Asteroid Belt

By Jean-Marc Petit, A. Morbidelli, J. Chambers. 2001

215 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Constructing the secular architecture of the solar system II: The terrestrial planets (2009, unknown): “Thus, we need to adopt the strategy introduced by Petit et al. (2001).”
The fossilized size distribution of the main asteroid belt (2003, methodology): “…et al., 2001; Scott, 2002, 2004)dynamical modeling work suggests their families would have likely be dispersed via encounters with planetary embryos(Petit et al., 2001)and/or sweeping resonances produced the dissipation of the gas component of the disk an the dynamical evolution of Jupiter…”
Terrestrial planet formation with strong dynamical friction (2006, background): “Thus, as also noted by other researchers (e.g., Petit et al., 2001; Chambers and Cassen, 2002), if no other mechanisms are invoked to enhance the eccentricity and inclination of Jupiter and Saturn after the formation of the terrestrial planets, they must start out with e and i larger than their…”
Water delivery and giant impacts in the 'Grand Tack' scenario (2014, unknown): “In the classical scenario, the distribution of planetesimals and embryos would have extended into the asteroid belt region, and the current population of asteroids is all that remains following the dynamical depletion of that region by the scattering effects of planetary embryos and dynamical resona”
The naked planet Earth: Most essential pre-requisite for the origin and evolution of life (2013, background): “Additionally, accretion event of asteroids seems to be stochastic event (e.g., Morbidelli et al., 2000; Petit et al., 2001).”
Toward Planetesimals: Dense Chondrule Clumps in the Protoplanetary Nebula (2008, background): “Model studies (e.g., Petit et al 2001, Kenyon and Bromley 2004, 2006; Bottke et al 2005; Chambers 2004,2006; Weidenschilling and Cuzzi 2006) suggest that the collisional stage occurred after dispersal of the nebula gas allowed the orbital eccentricities of primitive bodies to grow.”
The primordial excitation and clearing of the asteroid belt—Revisited (2006, methodology): “The Petit et al. (2001) work used the most advanced simulations possible with the computers available at the time and, as such, was a ground-breaking demonstration of the effects of planetary embryos on the primordial asteroid belt.”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, methodology): “1 shows the dynamical evolution of the embryos prior to the formation of Jupiter, which was set somewhat arbitrarily to 10 Myr.”
Oort cloud and Scattered Disc formation during a late dynamical instability in the Solar System (2012, unknown): “e of 0.04. However, it matches its current secular properties and at its secular maximum it is 0.06. The migration was accomplished by interpolation of the planets’ orbital elements with SWIFT RMVS3 (Petit et al., 2001; Brasser et al., 2009; Morbidelli et al., 2010). During this migration we kept th”
Asteroids Were Born Big (2009, background): “The embryos-in-the-Asteroid-belt-model in Wetherill (1992) does not only explain the depletion of the Asteroid belt but also the final orbital excitation of eccentricities and inclinations of the surviving asteroids and the radial mixing of bodies of different taxonomic types (Petit et al., 2001).”
Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “Resident planetary embryos in the belt can efficiently excite and deplete the belt (Wetherill, 1992; Chambers and Wetherill, 2001; Petit et al., 2001; O’Brien et al., 2007), although in many simulations embryos survive after the terrestrial planets have formed, in conflict with the observed Solar Sy”
The origin of water on Mars (2002, methodology): “The source is consistent with current understan of the water content of the asteroid belt as informed by chondritic meteorite record (Robert, 2001), and with the r of the giant planets in clearing the primordial asteroid b (Petit et al., 2000).”
Building the terrestrial planets: Constrained accretion in the inner Solar System (2009, background): “(Wetherill 1992; Chambers & Wetherill 2001; Petit et al. 2001; O’Brien et al. 2007), although other models do exist (e.g., Lecar & Franklin 1997; Nagasawa et al. 2000).”
Building Terrestrial Planets (2012, background): “lanetesimals typically remain in the asteroid belt on stable orbits at the end of the terrestrial planet formation process and all embryos are ejected from the belt in most, but not all, simulations (Petit et al 2001; O'Brien et al. 2007). The depletion of the belt by embryos and their subseque”
EVIDENCE FROM THE ASTEROID BELT FOR A VIOLENT PAST EVOLUTION OF JUPITER's ORBIT (2010, background): “…excitation of the asteroid belt occurred during the terrestrial planets formation process, due to the combination of perturbationsfrom resident planetary embryos and Jupiter (Wetherill, 1992; Chambers and Wetherill, 1998; Petit et al., 2001; Raymond et al., 2006; O’Brien et al., 2006, 2007).”
A Decreased Probability of Habitable Planet Formation around Low-Mass Stars (2007, background): “Indeed, the combined effects of embryo scattering and perturbations from Jupiter and Saturn are thought to be the cause of the depletion of the Solar System’s asteroid belt (Wetherill 1992; Chambers & Wetherill 2001; Petit et al. 2001).”