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

Solar and Stellar Astrophysics