Yarkovsky/YORP chronology of asteroid families

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In search of the source of asteroid (101955) Bennu: Applications of the stochastic YORP model (2015, methodology): “Finally, during collisional reorientation and mass shedding events, we assume the shape of the model asteroid has changed enough that a new shape function should be chosen from the available inventory of possibilities, as discussed in detail in Vokrouhlický et al. (2006a) (see also Appendix A).”
Asteroid family ages (2015, methodology): “The interpretation of this gap as a consequence of the interaction between the YORP and the Yarkovsky effect, as proposed in (Vokrouhlický et al., 2006b), is plausible and widely accepted, but a model capable of predicting the timescales of this evolution is not available.”
Rubble Pile Asteroids (2018, background): “ of asteroids that are driven into spin-orbit resonances in the Main Belt (“Slivan States” - Slivan et al. 2002; Vokrouhlický et al. 2003) and in the way that asteroid families drift apart over time (Vokrouhlický et al. 2006, Nesvorný et al. 2015). The YORP-effect can also alter obliquities, effecti”