Rotational fission of contact binary asteroids

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Dynamics of rotationally fissioned asteroids: Source of observed small asteroid systems (2011, background): “While the rotation rate needed to surface fission the primary is the same as the secondary–the surface fission rate only depends on density (Scheeres, 2007), the rotational kinetic energy necessary to achieve that rotation rate is much higher, and a transfer of this much energy into the rotation sta”
Stability of the planar full 2-body problem (2009, background): “This can be seen in the paper (Scheeres 2007), where similar stability diagrams are given for relative equilibrium stability in a sphere-ellipsoid system.”
Spin-up of rubble-pile asteroids: Disruption, satellite formation, and equilibrium shapes (2012, background): “Bodies with irregular shapes, and very non-circular equators (a/b much greater than 1; meaning that they are prolate), would not be expected to survive in a stable dynamical configuration for long timescales (Scheeres, 2007).”
Scaling forces to asteroid surfaces: The role of cohesion (2010, background): “Past studies have focused on a sub-set of physical forces, mainly gravitational, rotational (inertial) effects, friction forces, and constitutive laws [19, 20, 21, 22, 44, 55, 60].”
On the shapes and spins of “rubble pile” asteroids (2009, background): “(2006) and Scheeres et al., (2006) the asteroid (66391) 1999 KW4, shown in the cover illustration, is remarkable in having an almost cons tant”