Data on the rotational characteristics of more than 300 asteroids are currently available and it is now clear that the distribution of the rotation rates is non-random. A plot of rotation rate against asteroid diameter shows large dispersion but is distinctly V-shaped. The minimum of this curve at ca. 120 km may separate primordial asteroids from their collision products. There is also evidence that rotation rate depends on type classification, and weak evidence that it may also depend on family membership. Recent bias-free observations suggest that the marked rise of rotation rate with decreasing diameter D for those asteroids with D < 120 km cannot be completely accounted for by observational selection effects. A significantly large subset of the small asteroids have exceptionally long rotation periods suggestive of either a different nature and origin, or a peculiar history. Models that have been proposed to account for these results are discussed.