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The high-energy radiation emitted by young stars can have a strong influenceon their rotational evolution at later stages. This is because internalphotoevaporation is one of the major drivers of the dispersal of circumstellardisks, which surround all newly born low-mass stars during the first fewmillion years of their evolution. Employing an internal EUV/X-rayphotoevaporation model, we have derived a simple recipe for calculatingrealistic inner disk lifetimes of protoplanetary disks. This prescription wasimplemented into a magnetic morphology-driven rotational evolution model and isused to investigate the impact of disk-locking on the spin evolution oflow-mass stars. We find that the length of the disk-locking phase has aprofound impact on the subsequent rotational evolution of a young star, and theimplementation of realistic disk lifetimes leads to an improved agreement ofmodel outcomes with observed rotation period distributions for open clusters ofvarious ages. However, for both young star-forming regions tested in our model,the strong bimodality in rotation periods that is observed in hPer could not berecovered. hPer is only successfully recovered, if the model is started from adouble-peaked distribution with an initial disk fraction of $65\,\%$. However,at an age of only $\sim 1\,\mathrm{Myr}$, such a low disk fraction can only beachieved if an additional disk dispersal process, such as externalphotoevaporation, is invoked. These results therefore highlight the importanceof including realistic disk dispersal mechanisms in rotational evolution modelsof young stars.

Linking circumstellar disk lifetimes to the rotational evolution of low-mass stars