An update on the YORP-Yarkowski evolution of asteroid families

According to Golubov & Scheeres (2018) the coupling between obliquity and spin rate evolution drives the rotation state of small bodies towards equilibria which can significantly influence the spin dynamics of asteroids. To have a full picture of this dynamics it is essential to consider the so-called Tangential YORP (TYORP) effect, caused by asymmetric light emission by boulders or other structures on the surface of an asteroid. Introducing these findings in a model which tracks the coupled orbital and rotational evolution of asteroid families, under the action of the Yarkowsky and YORP effects, we are able to recover the characteristic V-shape configuration in the semimajor axis vs absolute magnitude (H) space. The time evolution of a number of synthetic families is explored with this model looking in detail at different size regimes and considering the influence of mutual collisions between the members of the family. Looking at time snapshots of the V-shape evolution the YORP-eye hypothesis (Paolicchi and Knezevic, Icarus, 2016) is probed too.