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The early stage of stellar evolution is characterized by a star-disc lockingmechanism. The disc-locking prevents the star to spin its rotation up, and itstimescale depends on the disc lifetime. Some mechanisms can significantlyshorten this lifetime, allowing a few stars to start spinning up much earlierthan other stars. In the present study, we aim to investigate how theproperties of the circumstellar environment can shorten the disc lifetime. Wehave identified a few multiple stellar systems, composed of stars with similarmasses, which belong to associations with a known age. Since all parametersthat are responsible for the rotational evolution, with the exception ofenvironment properties and initial stellar rotation, are similar for allcomponents, we expect that significant differences among the rotation periodscan only arise from differences in the disc lifetimes. A photometric timeseriesallowed us to measure the rotation periods of each component, whilehigh-resolution spectra provided us with the fundamental parameters, $v\sin{i}$and chromospheric line fluxes. The rotation periods of the components differsignificantly, and the component B, which has a closer companion C, rotatesfaster than the more distant and isolated component A. We can ascribe therotation period difference to either different initial rotation periods ordifferent disc-locking phases arising from the presence of the close companionC. In the specific case of BD$-$21 1074, the second scenario seems to be morefavored. In our hypothesis of different disc-locking phase, any planet orbitingthis star is likely formed very rapidly owing to a gravitational instabilitymechanism, rather than core accretion. Only a large difference of initialrotation periods alone could account for the observed period difference,leaving comparable disc lifetimes.

Evidence from stellar rotation of enhanced disc dispersal: (I) The case of the triple visual system BD-21 1074 in the $\beta$ Pictoris association