The primordial excitation and clearing of the asteroid belt—Revisited
By D. O'Brien, A. Morbidelli, William Bottke. 2006
145 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/533a29a1f592235ec97faf3ff9392dfb6bf8bb64
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In Astronomy and Astrophysics
- A. Morbidelli
- D. Nesvorný
- William Bottke
- Kevin J. Walsh
- S. Raymond
- Harold Levison
- F. DeMeo
- A. Izidoro
Citations in the corpus
- Asteroids Were Born Big (2009, background): “By this process, 99% of the asteroids acquired an eccentricity that exceeded the value characterizing the stability boundary of the current Asteroid belt (O’Brien et al., 2007).”
- Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion (2017, background): “…excitation have been proposed, including excitation by local planetary embryos (Wetherill, 1992; Chambers and Wetherill, 2001; Petit et al., 2001; O’Brien et al., 2007), sweeping secular resonances (Lecar and Franklin, 1997; Zheng et al., 2017), and chaotic excitation by Jupiter and Saturn…”
- Dynamical erosion of the asteroid belt and implications for large impacts in the inner Solar System (2009, background): “What we mean by this is the time at which any primordial mass depletion and excitation has already taken place (see O’Brien et al., 2007), and any early orbital migration of giant planets has finished (Fernandez and Ip, 1984; Malhotra, 1993; Strom et al., 2005; Gomes et al., 2005; Minton and…”
- 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 Compositional Structure of the Asteroid Belt (2015, background): “Studies of sweeping secular resonances due to the dissipation of the solar nebula suffer dual problems of needing long (20 Myr) timescales of gas dissipation to deplete enough bodies, and then typically fail to reproduce the inclination distributions (see O’Brien et al., 2007).”