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We present a large-scale study of stellar rotation for T Tauri stars in theOrion Star-Forming Complex. We use the projected rotational velocity($v\sin(i)$) estimations reported by the APOGEE-2 collaboration as well asindividual masses and ages derived from the position of the stars in the HRdiagram, considering Gaia-EDR3 parallaxes and photometry plus diverseevolutionary models. We find an empirical trend for $v\sin(i)$ decreasing withage for low-mass stars ($0.4 M_{\odot} < M_{\ast} < 1.2 M_{\odot}$). Ourresults support the existence of a mechanism linking $v\sin(i)$ to the presenceof accreting protoplanetary disks, responsible for regulating stellar rotationin timescales of about 6 Myr, which is the timescale in which most of the TTauri stars lose their inner disk. Our results provide important constraints tomodels of rotation in the early phases of evolution of young stars and theirdisks.

Stellar Rotation of T Tauri stars in the Orion Star-Forming Complex