The collisional and dynamical evolution of the main-belt and NEA size distributions

By D. O'Brien, Richard Greenberg. 2005

166 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/e35c1c4bbdd586fc897c9db9efdee6d7c9f583c9

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Citations in the corpus

The primordial excitation and clearing of the asteroid belt—Revisited (2006, methodology): “The Petit et al. (2001) simulations, like our EJS simulations, considered an eccentric Jupiter and Saturn. The differences in the outcomes of these simulations [faster and stronger asteroid depletion in the Petit et al. (2001) simulations] can be explained by the facts that in Petit et al. (2001), t”
The global effects of impact-induced seismic activity on fractured asteroid surface morphology (2005, background): “At the same time, the lunar seismic experiments showed extremely high values for Q (Pandit and Tozer, 1970).”
Asteroids Were Born Big (2009, background): “Also, the ratio between the numbers of families with progenitors larger than 100 and 200 km, respectively, would be a factor of 4 larger than observed (O’Brien and Greenberg, 2005).”
THE IMPORTANCE OF SECONDARY CRATERING TO AGE CONSTRAINTS ON PLANETARY SURFACES (2006, background): “…of the effects of thermal re-emission and other processes on the SFD of NEAs smaller than 1 km has recently been completed (Bottke et al. 2005, O’Brien & Greenberg 2005), and both studies conclude that the SFD of small asteroids both in the main belt and NEAs continue to small sizes at a…”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “Since that time, an additional model has been sub ted (O’Brien and Greenberg, 2005) and another publishe (Cheng, 2004) .”
Size-frequency distributions of fragments from SPH/N-body simulations of asteroid impacts: Comparison with observed asteroid families (2007, result): “In contrast, comparisons between our family distribution estimates and the results of other main-belt evolution models (e.g., Durda et al., 1998; Cheng, 2004; O’Brien and Greenberg, 2005) indicate these models produce considerably more families from D > 100 km parent bodies than permitted by observa”