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Equal-mass stars in young open clusters and loose associations exhibit a widespread of rotation periods, which likely originates from differences in theinitial rotation periods and in the primordial disc lifetimes. We want toexplore if the gravitational effects by nearby companions may play anadditional role in producing the observed rotation period spread. We measurethe photometric rotation periods of components of multiple stellar systems andlook for correlations of the period differences among the components to theirreciprocal distances. In this paper, we analysed the triple system AU Mic + ATMic A&B in the 25-Myr beta Pictoris Association. We have retrieved from theliterature the rotation period of AU Mic (P = 4.85d) and measured fromphotometric archival data the rotation periods of both components of AT Mic (P= 1.19d and P = 0.78d) for the first time. Moreover, we detected a high rate offlare events from AT Mic. Whereas the distant component AU Mic has evolvedrotationally as a single star, the A and B components of AT Mic, separated byabout 27 AU, exhibit a rotation rate a factor 5 larger than AU Mic. Moreover,the A and B components, despite have about equal mass, show a significantdifference (about 40%) between their rotation periods. A possible explanationis that the gravitational forces between the A and B components of AT Mic (thatare a factor about 7.3 x 10^6 more intense than those between AU Mic and ATMic) have enhanced the dispersal of the AT Mic primordial disc, shortening itslifetime and the disc-locking phase duration, making the component A and B ofAT Mic to rotate faster than the more distant AU Mic. We suspect that adifferent level of magnetic activity between the A and B components of AT Micmay be the additional parameter responsible for the difference between theirrotation periods.

The triple system AT Mic AB + AU Mic in the beta Pictoris Association