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Modeling Asteroid Impact Dynamics: Catastrophic Disruption of Three Distinct Structure Types

Introduction. This paper reports the outcome of highspeed collision experiments in three distinct structure types. The purpose was to make qualitative and quantitative comparisons of possible asteroid structure types, specifically aggregates (to simulate a “rubble pile” body), fractured bodies and solid bodies. The benefits of such a study are numerous and will help to demonstrate the types of processes that form the space environment that surrounds the Earth. Helping to shed light on the collision history of our solar system, these experiments could also help us to predict future impact events. There have been numerous impact experiments in the past, but relatively few have dealt with the comparison of impacts of similar energy into distinct structure types. All of the bodies consisted of a porphorytic basalt with olivine phenocrysts, in order to best simulate the consistency of a chondritic meteorite [1]. The experiments were conducted at the Ames Vertical Gun Range (AVGR) in October 2001 and June 2002. Qualitatively, it was observed that there was much more localization of the impact area in the collisions with the fractured and aggregate bodies than was observed in the solid body collision. Quantitatively, projectile speeds were measured to be similar to the average in the asteroid belt, and the impact energies were measured to be between 4.96x10 /kg and 1.20x10 /kg. The percentages of intact mass of the target bodies that were not directly impacted were 42.09%, 79.38% and 98.74% for the solid, fractured, and aggregate bodies respectively. These numbers give us a good insight into the propagation of shock waves in the different solids. This information also supports some of the current theories concerning rubble pile asteroids, and their ability to survive comparatively large impact events [2]. In this study, structure type appears to be the most influential factor concerning the disruption event’s outcome.