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Current amount of ~500 asteroid models derived from the disk-integratedphotometry by the lightcurve inversion method allows us to study not only thespin-vector properties of the whole population of MBAs, but also of severalindividual collisional families. We create a data set of 152 asteroids thatwere identified by the HCM method as members of ten collisional families, amongthem are 31 newly derived unique models and 24 new models with well-constrainedpole-ecliptic latitudes of the spin axes. The remaining models are adopted fromthe DAMIT database or the literature. We revise the preliminary familymembership identification by the HCM method according to several additionalcriteria - taxonomic type, color, albedo, maximum Yarkovsky semi-major axisdrift and the consistency with the size-frequency distribution of each family,and consequently we remove interlopers. We then present the spin-vectordistributions for eight asteroidal families. We use a combined orbital- andspin-evolution model to explain the observed spin-vector properties of objectsamong collisional families. In general, we observe for studied families similartrends in the (a_p, \beta) space: (i) larger asteroids are situated in theproximity of the center of the family; (ii) asteroids with \beta>0{\deg} areusually found to the right from the family center; (iii) on the other hand,asteroids with \beta<0{\deg} to the left from the center; (iv) majority ofasteroids have large pole-ecliptic latitudes (|\beta|\gtrsim 30{\deg}); andfinally (v) some families have a statistically significant excess of asteroidswith \beta>0{\deg} or \beta<0{\deg}. Our numerical simulation of the long-termevolution of a collisional family is capable of reproducing well the observedspin-vector properties. Using this simulation, we also independently constrainthe age of families Flora (1.0\pm0.5 Gyr) and Koronis (2.5-4 Gyr).

An anisotropic distribution of spin vectors in asteroid families