  Rotation is one of the key stellar parameters which undergo substantial
evolution during the stellar lifetime, in particular during the early stages.
Stellar rotational periods can be determined on the basis of the periodic
modulation of starlight produced by non-uniformities on the surface of the
stars, due to manifestation of stellar activity. We present the results of an
extensive search for rotational periods among NGC 2264 cluster members, based
on photometric monitoring using the CoRoT satellite, with a particular
attention to the distribution of classical and weak-line T-Tauri stars. NGC
2264 is one of the nearest and best studied star forming region in the solar
neighbourhood, with an estimated age of 3 Myr, and is the object of a recent
simultaneous multiband campaign including a new CoRoT observation with the aim
to assess the physical origin of the observed variability. We find that the
rotational distributions of classical and weak-line T-Tauri star are different,
suggesting a difference in the rotational properties of accreting and
non-accreting stars.
