Other
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.1606w&link_type=abstract
American Astronomical Society, DPS meeting #39, #16.06; Bulletin of the American Astronomical Society, Vol. 39, p.440
Other
Scientific paper
Recent theoretical and observational research has suggested that tidal disruption is not a sufficient mechanism to produce all of the kilometer-sized binary asteroids in the inner solar system (Walsh & Richardson 2007, Pravec et al. 2006). We present simulation results from the slow spin-up of strengthless bodies in a way designed to mimic thermal spin-up effects acting on small asteroids (the so-called YORP effect). These simulations employ cohesionless bodies represented by identical self-gravitating spheres. The spin rate of these bodies is increased slowly allowing time for transient responses of the body to decay. The simulations track the changes in shape and spin to the bodies as their spin rate increases, as well as the fate of particles which are ejected. Included in this work are simulations with rubble piles made up of small rigid aggregates of two-particle "dumbbells" rather than simply single spherical particles. This provides the body with some extra resistance against flows of particles during re-shaping and mass loss.
We find that binary formation is a possible outcome from slow spin-up and discuss the parameters leading to this result as well as the properties of the binaries produced. We also discuss the shapes of bodies in relation to the Jacobi sequence and other theoretical equilibrium limits as they approach rotational disruption and reshaping.
DCR and KJW acknowledge support from NSF grants AST0307549 & AST0708110. PM acknowledges support of the ESA Advanced Concepts Team on the basis of the Ariadna study 07/4111, "Asteroid Centrifugal Fragmentation".
References:
Pravec, P. et al. 2006. Icarus 181, 63.
Walsh, K.J., Richardson, D.C. 2007. Icarus, in press.
Michel Pascal
Richardson Chris D.
Walsh Kevin J.
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