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We present the combined results of three photometric monitoring campaigns targeting very low mass (VLM) stars and brown dwarfs in the young open cluster IC4665 (age ∼40 Myr). Each of our observing runs covers time‐scales of ∼5 d in the seasons 1999, 2001 and 2002, respectively. In all three runs, we observe ∼100 cluster members, allowing us for the first time to put limits on the evolution of spots and magnetic activity in fully convective objects on time‐scales of a few years. For 20 objects covering masses from 0.05 to  0.5 M ⊙  , we detect a periodic flux modulation, indicating the presence of magnetic spots co‐rotating with the objects. The detection rate of photometric periods (∼20 per cent) is significantly lower than in solar‐mass stars at the same age, which points to a mass dependence in the spot properties. With two exceptions, none of the objects exhibits variability and thus spot activity in more than one season. This is contrary to what is seen in solar‐mass stars and indicates that spot configurations capable of producing photometric modulations occur relatively rarely and are transient in VLM objects. The rotation periods derived in this paper range from 3 to 30 h, arguing for a lack of slow rotators among VLM objects. The periods fit into a rotational evolution scenario with pre‐main sequence contraction and moderate (40–50 per cent) angular momentum losses due to wind braking. By combining our findings with literature results, we identify two regimes of rotational and magnetic properties, called C‐ and I‐sequence. Main properties on the C‐sequence are fast rotation, weak wind braking, Hα emission and saturated activity levels, while the I‐sequence is characterized by slow rotation, strong wind braking, no Hα emission and linear activity‐rotation relationship. Rotation rate and stellar mass are the primary parameters that determine in which regime an object is found. We outline a general scheme to understand rotational evolution for low‐mass objects in the context of these two regimes and discuss the potential as well as the problems of this picture.

Long‐term monitoring in IC4665: fast rotation and weak variability in very low mass objects