  We present a comparison between the rotation period distributions of
solar-type single stars and primary stars in close binaries (0.1 AU ~< a ~< 5
AU) in the young (150 Myr) open cluster M35 (NGC 2168). We find that the
primary stars in the close binaries rotate faster than the single stars, on
average. The differences in the means and medians between the period
distributions are statistically significant at the 99.9% level or higher. The
faster rotation among the primary stars in close binaries is not due to tidal
synchronization as tidally evolved stars are excluded from the comparison. We
discuss this result in the context of different early-evolution accretion
processes and star-disk interactions for single stars and stars in close
binaries.
