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Massive stars are strong sources of far-ultraviolet radiation that can behostile to the evolution of protoplanetary disks, driving mass loss by externalphotoevaporation and shortening disk-dissipation timescales. Their effect mayalso reduce the timescale of angular momentum exchanges between the disk andhost star during the early pre-main-sequence phase. To improve ourunderstanding of the environmental influence on the rotational history ofstars, we developed a model that considers the influence of the localfar-ultraviolet radiation on the spin evolution of low mass stars. Our modelincludes an assumption of disk-locking, which fixes the rotation rate duringthe star-disk-interaction phase, with the duration of this phase parametrisedas a function of the local far-ultraviolet radiation and stellar mass (in therange 0.1--1.3 M$_\odot$). In this way, we demonstrate how the feedback frommassive stars can significantly influence the spin evolution of stars andexplain the mass-dependency observed in period-mass distributions of youngregions like Upper Sco and NGC 2264. The high far-ultraviolet environments ofhigh-mass stars can skew the period distribution of surrounding stars towardsfast-rotation, explaining the excess of fast-rotating stars in the open clusterh Per. The proposed link between rotation and the pre-main-sequence environmentopens new avenues for interpreting the rotational distributions of young stars.For example, we suggest that stellar rotation may be used as a tracer for theprimordial ultraviolet irradiation for stars up to $\sim$1 Gyr, which offers apotential method to connect mature planetary systems to their birthenvironment.

The influence of the environment on the spin evolution of low-mass stars. I. External photoevaporation of circumstellar disks