Disruptive Impacts into Small Asteroids

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Scientific paper

Inversion of radar images (Ostro et al 1990, Science 248:1523; Hudson and Ostro 1994, Science 263:940--943) of the Earth-crossing asteroid 4769 Castalia yielded a shape model bifurcated into distinct, km-sized lobes. We construct a smooth particle hydrodynamics (SPH) rendering in the manner described by Asphaug et al (Icarus 120:158--184) using 2.1g/cm(3) rock seeded with explicit flaws governing crack growth (Benz and Asphaug 1995, Comp. Phys. Comm. 87:235--265). We subject this rocky target to a variety of impacts (altering impactor velocity, trajectory, energy, composition, etc.) and also explore icy and shattered targets. An 8m radius impactor at 5 km/s causes extensive fragmentation (white particles, below) and cracks the lobes apart. 12% of the target escapes in this impact, and Delta V~ 3cm/s for the non-escaping remainder. A 3m impactor creates a ~ 200m diameter noncatastrophic crater plus radial cracks; the disruption threshold for an irregular rock of this size is thus Q(*~) 5x 10(5) erg/g. Because Castalia may have formed by low-velocity collision between two separate objects in the first place, we next replace the region between the lobes with zero-strength, low-density material. The impacted lobe suffers nearly total damage, while the other lobe is shielded by the discontinuity. To determine the final stage of impact evolution, we perform N-body gravitational calculations to determine the trajectories of ejecta and larger fragments. This research presumes Castalia to be ``typical" in some way. Future work will include radar and visual shape determinations for asteroids Toutatis, Eros and Miranda. This research is supported in part by NASA grant NAGW-3904.

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