Icarus for March (vol. 446) contains:
Oszkiewicz, D. Bartczak, P. Colazo, M. et al. Asteroid phase curve modeling with empirical correction for shape and viewing geometry Art 116886 .2025.116886
Kurosaki, K. Arakawa, M. Numerical simulation of impact cratering and induced seismic waves in sand targets Art 116874 .2025.116874
Phase curves are the slight variances in light and reflectivity that occur as we shine a different light on bodies. Light shining at an angle (high-phase) will reflect slightly differently than light shining from ‘dead on’ (low-phase). We can exploit this difference to tell us of the body in question. For asteroids, different phase curves will correspond with different albedos: the dark carbonaceous chondrites will have different phase curves than the lighter ordinary (more stony) chondrites. But this difference is more comprehensible and understood for smooth spheres. As we introduce roughness (i. e., a surface of regolith) and irregular shape (‘potatos’ in space), the relationship becomes more complicated.
Speaking of regolith, all but the smallest asteroids have it. Large asteroids (many kilometers across) in particular have the gravity to retain fine sand. But even smaller asteroids (e. g., Ryugu and Bennu) have some regolith, just not the lighter stuff. Kurosaki and Arakawa attempt to put more decimal places on our understanding of this regolith as meteors impact it: what are the dynamics of cratering?