Planets in the asteroid belt

By J. Chambers, G. Wetherill. 2001

146 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/8689fa1a659d5dc1038a8b0e16795fc46cc996b7

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In Astronomy and Astrophysics

Citations in the corpus

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).”
Asteroids Were Born Big (2009, background): “The combination of their mutual perturbations and of the dynamical action of resonances with Jupiter eventually removed them from the Asteroid belt (Chambers and Wetherill, 2001; O’Brien et al., 2006).”
Making other earths: dynamical simulations of terrestrial planet formation and water delivery (2003, result): “An eccentric Jupiter clears out the asteroid region much more quickly than a low eccentricity Jupiter, both by increased ejection efficiency and, more significantly, a large increase in the number of objects which collide with the Sun, as expected from the results of Chambers and Wetherill (2001) .”
Equilibration in the aftermath of the lunar-forming giant impact (2007, background): “In particular, while >10% of the planetary embryos in 467 the asteroid belt that are removed by mean-motion resonances collide with the terrestrial 468 planets, those embryos that are removed by the secular resonance at 2.1 AU are 469 dynamically excited so rapidly that they almost always collide wi”
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).”
Building Terrestrial Planets (2012, methodology): “However, numerical simulations (Chambers and Wetherill 2001; Raymond et al. 2004, 2005; O’Brien et al. 2006) show that the dynamical evolution is very different in the terrestrial planet region versus the asteroid belt.”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “Models describing the evolution of planetary embryos and planetesimals in the inner Solar System have been described by several groups (Agnor et al., 1979; Chambers and Wetherill 1998; 2001; Chambers and Cassen, 2002).”
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”
Oxygen isotope evidence for rapid mixing of the HED meteorite parent body (2004, background): “In fact several hundreds of planetary embryos of the size of Vesta may once have existed in what is now the asteroid belt [10].”
The Primordial Excitation and Clearing of the Asteroid Belt (2001, methodology): “We start with data for the orbital evolution of the embryos obtained by Chambers and Wetherill (1998, 2001) and Chambers (1998).”
Planetary accretion in the inner Solar System (2004, background): “Numerical simulations show that all embryos in the asteroid region are likely to be lost in this way, along with the great majority of smaller asteroids, once the giant planets form [73].”
Terrestrial planet formation with strong dynamical friction (2006, methodology): “For example, Chambers and Wetherill (1998, 2001) find that an embryo remains in the asteroid belt region in about 1/3 of their simulations.”
Evolution of a habitable planet (2003, background): “The timing of the delivery of volatiles, the size of asteroid-like volatile reservoirs, and the efficiency with which the volatiles are delivered depend sensitively on the locations, sizes, and initial orbital eccentricities of the giant planets (Chambers & Wetherill 2001).”
The fossilized size distribution of the main asteroid belt (2003, background): “Despite the claim that Durda et al. (1998)can reproduce the main belt size distribution, we find their best solution forNrem andQ∗D to be unrealistic. Our computa tions indicate theDurda et al. (1998) best-fit case yields 4 D > 100 km asteroid disruptions over the last 3.”
Gravitational Aggregates: Evidence and Evolution (2002, background): “(1998) showed that the postencounter spin and ellipticity of the progenitor are correlated with the preencounter values: A prograde progenitor spins up a bit and becomes more elongated, a retrograde progenitor spins down and becomes more spherical. Scheeres et al. (2000) used a combination of analyt”
The primordial excitation and clearing of the asteroid belt—Revisited (2006, background): “…exciting and scattering one-another and the asteroids into resonances with Jupiter and Saturn (e.g., Wetherill, 1992; Chambers and Wetherill , 1998; Chambers and Wetherill, 2001; Petit et al., 2001), are able to reasonably reproduce all of the observed characteristics of the asteroid belt in the…”
Making More Terrestrial Planets (2001, background): “Conversely, several of simulations of Wetherill (1986), Cox and Lewis (1980), Lec and Aarseth (1986), Agnor et al.”