On the shapes and spins of “rubble pile” asteroids

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THE ACTIVE ASTEROIDS (2011, background): “A major complication is that YORP torques can change not just the rotation state but the shape of an asteroid, as material slides, bounces or rolls towards the rotational equator on its way to escape (e.g. Harris et al., 2009, Statler 2009).”
Extreme sensitivity of the YORP effect to small-scale topography (2009, methodology): “For definiteness I adopt the mean Hapke parameters for S-class asteroids given by Helfenstein and Veverka (1989):a single-scattering albedow = 0.23, and a phase function expanded to 6th order in Legendre polynomials with a width parameterξ = −0.35.”
Rubble Pile Asteroids (2018, background): “…rapidly spinning asteroids that have satellites, suggesting that this is an end-state of a spin-up and binary formation process (Walsh et al. 2008, Harris et al. 2009, Scheeres et al. 2016), but is also found around at least one non-binary with moderate spin - Bennu the target of NASA’s…”