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Seismic shaking is an attractive mechanism to explain the destabilisation ofregolith slopes and the regolith migration found on the surfaces of asteroids(Richardson et al. 2004; Miyamoto et al. 2007). Here, we use a continuummechanics method to simulate the seismic wave propagation in an asteroid.Assuming that asteroids can be described by a cohesive core surrounded by athin non-cohesive regolith layer, our numerical simulations of vibrationsinduced by micro-meteoroids suggest that the surface peak ground accelerationsinduced by micro-meteoroid impacts may have been previously under-estimated.Our lower bound estimate of vertical accelerations induced by seismic waves isabout 50 times larger than previous estimates. It suggests that impact eventstriggering seismic activity are more frequent than previously assumed forasteroids in the kilometric and sub-kilometric size range. The regolith loftingis also estimated by a first order ballistic approximation. Verticaldisplacements are small, but lofting times are long compared to the duration ofthe seismic signals. The regolith movement has a non-linear dependence on thedistance to the impact source which is induced by the type of seismic wavegenerating the first movement. The implications of regolith concentration inlows of surface acceleration potential are also discussed. We suggest that theresulting surface thermal inertia variations of small fast rotators may inducean increased sensitivity of these objects to the Yarkovsky effect.

Micro-meteoroid seismic uplift and regolith concentration on kilometric scale asteroids