Serna, JavierJavierSernaHernandez, JesusJesusHernandezKounkel, MarinaMarinaKounkelManzo-Martinez, EzequielEzequielManzo-MartinezRoman-Lopes, AlexandreAlexandreRoman-LopesRoman-Zuniga, Carlos G.Carlos G.Roman-ZunigaGracia Batista, MariaMariaGracia BatistaPinzon, GiovanniGiovanniPinzonCalvet, NuriaNuriaCalvetBriceno, CesarCesarBricenoTapia, MauricioMauricioTapiaSuarez, GenaroGenaroSuarezPena Ramirez, KarlaKarlaPena RamirezStassun, Keivan G.Keivan G.StassunCovey, KevinKevinCoveyVargas-Gonzalez, J.J.Vargas-GonzalezFernandez-Trincado, Jose G.Jose G.Fernandez-Trincado2025-12-302025-12-3020211538-4357https://hdl.handle.net/20.500.12740/24065We 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 (0.4M(circle dot) < M-* < 1.2M(circle dot)). Our results support the existence of a mechanism linking v sin(i) to the presence of accreting protoplanetary disks, responsible for regulating stellar rotation on 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.Acceso AbiertoANGULAR-MOMENTUM EVOLUTIONMAIN-SEQUENCE STARSLOW-MASS STARSSIGMA-ORIONISYOUNG STARSPHOTOMETRIC VARIABILITYDIFFERENTIAL ROTATIONSPECTRAL-ANALYSISNEBULA CLUSTERVELOCITIEShttp://dx.doi.org/10.3847/1538-4357/ac300a