Abstract
Abstract Porous structure is common in the asteroids and satellites of the outer planets. In order to study the relationship between the structure of small bodies and their thermal and collisional evolution, we performed impact disruption experiments on porous sintered targets using a light-gas gun at velocities ranging from 10 to 100 m/s. The sintered glass bead targets were prepared to have roughly the same porosity but with different compressive strengths, ranging over an order of magnitude, by controlling sintering duration and temperature. The results of the impact experiments show that the targets of higher compressive strength have higher impact strengths. However, compared to previous results on impact disruption of porous sintered targets with a collisional velocity of approximately 6 km/s, the values of impact strength in this study were found to be lower by an order of magnitude.
Highlights
Since the end of the accretion phase of the Solar System approximately 4.5 Gyr ago, collisional disruptions have played various roles in the formation and evolution processes of the planetary system
Possible reasons for the very low values of Q* in the present results may be: (1) the lower the impact velocity, the larger the mass of the projectile needs to be in order to attain the same energy density (Q) as a higher impact velocity and, a smaller degree of attenuation of the stress wave in the targets, despite the porosity, due to the small contrast in size between the projectiles and targets; (2) difference in the dependence of the initial peak pressure on impact velocity between the high- and low-velocity impact disruption; (3) breakup of the largest fragments when they hit the wall of the chamber
Summary We succeeded in producing sintered glass bead targets that had roughly the same porosity but different compressive strength
Summary
Since the end of the accretion phase of the Solar System approximately 4.5 Gyr ago, collisional disruptions have played various roles in the formation and evolution processes of the planetary system. The outcomes of collisional disruptions have been studied for decades by laboratory experiments, scaling approaches, and numerical simulations (Fujiwara et al, 1989; Holsapple et al, 2002). The materials used in laboratory experiments were mostly non-porous rocks and ices. Porous structure has since been found to be common among asteroids (e.g., Britt et al, 2002; Fujiwara et al, 2006) and, the outcomes of collisional disruption of porous bodies have become of great significance for studying the origins and collisional evolution of small bodies. Q* generally depends on material strength (Holsapple et al, 2002); porosity plays a complicated role.
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