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We report the analysis of the rotational properties of our sample of HerbigAe/Be (HAeBe) and related stars for which we have obtained high-resolutionspectropolarimetric observations. Using the projected rotational velocitiesmeasured at the surface of the stars, we have calculated the angular momentumof the sample and plotted it as a function of age. We have then compared theangular momentum and the vsini distributions of the magnetic to thenon-magnetic HAeBe stars. Finally we have predicted the vsini of thenon-magnetic, non-binary ("normal") stars in our sample when they reach theZAMS, and compared them to various catalogues of the vsini of main-sequencestars. First, we observe that magnetic HAeBe stars are much slower rotatorsthan normal stars, indicating that they have been more efficiently braked thanthe normal stars. In fact, the magnetic stars have already lost most of theirangular momentum, despite their young ages (lower than 1 Myr for some of them).Secondly, our analysis suggests that the low mass (1.5 < M < 5 Msun) normalHAeBe stars evolve with constant angular momentum towards the ZAMS, while thehigh-mass normal HAeBe stars (M > 5 Msun) are losing angular momentum. Wepropose that winds, which are expected to be stronger in massive stars, are atthe origin of this phenomenon.

A high-resolution spectropolarimetric survey of Herbig Ae/Be stars - II. Rotation