Low-velocity impact response of lunar and Martian regolith simulants: Implications for lunar and Martian surface explorations.

This article focuses on experimental investigations of the granular mechanics of lunar and Martian regolith simulants under low-velocity impact conditions to better understand crater formation relevant to extraterrestrial exploration. Using high-fidelity simulants—LHS-1 for lunar highlands, LMS-1 for lunar mare, and MGS-1 for Martian regolith—alongside terrestrial silica sand (T-8), the study measured crater depths formed by dropping a 10-mm alumina sphere at velocities of 0.44–0.70 m/s. Results showed that crater depths in lunar highlands (LHS-1) and Martian simulants (MGS-1) were significantly greater than those in lunar mare (LMS-1) and terrestrial sand, attributed primarily to differences in cohesion and internal friction rather than particle size or porosity alone. The study’s power-law scaling indicates that lunar and Martian regolith layers offer less resistance to impact than terrestrial sand, with implications for optimizing landing, drilling, sampling, and construction strategies on these planetary surfaces.