mass loss associated with spin-off events (e.g., @holsapple10 [@hirabayashi15]) are processes that would eject a population of rocks and boulders from an asteroid surface. Eventually, this material would be ejected from the asteroid’s vicinity or it would return to hit the asteroid surface. A rubble pile asteroid can be formed following a disruptive collision of two large bodies, including a phase of re-accumulation from previously disrupted but gravitationally bound material [@michel13; @walsh18; @walsh19]. Late stages of re-accumulation involves low velocity impacts onto the asteroid surface. Impacts with objects in solar orbit have a mean relative velocity of $\sim 5$ km/s [@bottke94]. In comparison, a gravitational bound object would impact the asteroid surface at much lower velocity, less than the escape velocity which is $\sim 20$ cm/s for an 500 m diameter object such as Asteroid 101995 Bennu [@scheeres19]. These would be low velocity impacts into surface regolith or rubble at low gravitational acceleration and would include encounters at low or at grazing incidence angle because the projectiles were previously in orbit. Due to its orbital angular momentum, this would also be true of most material that was thrown off the asteroid during spin-off events. Experiments of low velocity and normal 