We present a comparison between the rotation period distributions of solar-type single stars and primary stars in close binaries ( 0.1 AU \lesssim a \lesssim 5 AU ) in the young ( \sim 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 .