The depletion of objects in the central part of an asteroid family,
which can be observed in the absolute magnitude vs. semimajor axis,
can be explained in terms of a coupling of the YORP and Yarkovsky
effects (Paolicchi and Knezevic, Icarus, 2016). In particular, it can
be ascribed to the obliquity evolution caused by YORP and on how it
influeces the Yarkovsky drift.With this work we intend to improve the
modeling of YORP-Yarkovsky evolution of asteroid families exploiting a
model which tracks the evolution of the spin vector of small
asteroids, including also the effects of collisions on the YORP
induced obliquity evolution. This allows a better modeling of the
asteroid spin evolution.In these preliminary steps, we will first
consider a few model families simulating their time evolution in the
magnitude vs. semimajor axis plots. The obtained results will be then
compared with observed families to determine and tune the intensity of
the effect
