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Models of rotating single stars can successfully account for a wide varietyof observed stellar phenomena, such as the surface enhancements of N and He.However, recent observations have questioned the idea that rotational mixing isthe main process responsible for the surface enhancements, emphasizing the needfor a strong and conclusive test.  We investigate the consequences of rotational mixing for massivemain-sequence stars in short-period binaries. In these systems the tides spinup the stars to rapid rotation. We use a state-of-the-art stellar evolutioncode including the effect of rotational mixing, tides, and magnetic fields. Wediscuss the surface abundances expected in massive close binaries (M1~20 solarmasses) and we propose using such systems to test the concept of rotationalmixing. As these short-period binaries often show eclipses, their parameterscan be determined with high accuracy, allowing for a direct comparison withbinary evolution models.  In more massive close systems (M1~50 solar masses, Porb<~2 days) we find thathelium is efficiently mixed throughout the envelope. The star remains blue andcompact during the main-sequence phase. It stays within its Roche lobe while itgradually becomes a helium star. It is the less massive star, in which theeffects of rotational mixing are less pronounced, which fills its Roche lobefirst. We propose that this evolution path provides an alternative channel forthe formation of tight Wolf-Rayet binaries with a main-sequence companion andmight explain massive black hole binaries such as the intriguing system M33X-7.

Rotational mixing in massive binaries: detached short-period systems