The formation of asteroid satellites in large impacts: Results from numerical simulations

By D. Durda, William Bottke, B. Enke, W. Merline, E. Asphaug, Derek C. Richardson, Z. Leinhardt. 2004

183 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/41d5c41b8ebd8b583be00557185434992d099040

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Citations in the corpus

COLLISIONS BETWEEN GRAVITY-DOMINATED BODIES. I. OUTCOME REGIMES AND SCALING LAWS (2011, methodology): “Our simulations resolve over a decade in fragment size, comparable to SPH simulations using an order of magnitude more particles (Durda et al. 2004).”
Full numerical simulations of catastrophic small body collisions (2008, methodology): “In the first phase, the time scale for the propagation of the shock wave is determined by the target size divided by the sound speed of the material (few to 10s of seconds for a nonporous rocky target with RT 50 km).”
Rubble Pile Asteroids (2018, background): “Therefore most efforts include a handoff from hydrodynamics to Nbody gravity particle codes (Michel et al. 2001,2002,2003,2004, Durda et al. 2004, 2007, Benavidez et al. 2015).”
Yarkovsky/YORP chronology of asteroid families (2006, methodology): “This geometry has yet to be observed in numerical simulations of asteroid collisions (e.g., Durda et al., 2004 ) nor would it be expected from heuristic arguments.”
The fossilized size distribution of the main asteroid belt (2003, background): “For example because super-catastrophic disruption events are exp to produce numerous small fragments (Michel et al., 2001, 2003; Durda et al., 2004a, 2004b), Tanga et al. may undere timate the number of observedD > 100 km breakup events particularly if numerous family members are below the tection…”
Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu (2014, background): “at experienced a collision (Campins et al. 2010; Walsh et al. 2013). Similarly, the large multiple systems examined by Marchis et al. (2008a,b) were presumably formed by large collision events (e.g., Durda et al. 2004). One would expect these smashed up target worlds, with porosity added by the frag”
In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model (2015, background): “Reasons that the largest remnant would be displaced from the family center include peculiarities in the nature of the disruption event (e.g., Durda et al., 2004) and/or the dynamical evolution of the largest remnant via the Yarkovsky effect (e.g., Warner et al., 2009) or asteroid close encounters…”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, methodology): “To determine how many families fit this criteria, B05 used hydrocode simulations of asteroid collisions (Durda et al., 2004) to estimate the amount of material in each family located below the observational detection limit.”