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Most existing studies of the angular momentum evolution of young stellarpopulations have focused on the youngest (1-3 Myr) T Tauri stars. In contrast,the angular momentum distributions of older T Tauri stars (4-10 Myr) have beenless studied, even though they hold key insight to understanding stellarangular momentum evolution at a time when protoplanetary disks have largelydissipated and when models therefore predict changes in the rotationalevolution that can in principle be tested. We present a study of photometricvariability among 1,974 confirmed T Tauri members of various sub-regions of theOrion OB1 association, and with ages spanning 4-10 Myr, using opticaltime-series from three different surveys. For 564 of the stars (~32% of theweak-lined T Tauri stars and ~13% of the classical T Tauri stars in our sample)we detect statistically significant periodic variations which we attribute tothe stellar rotation periods, making this one of the largest samples of T Tauristar rotation periods yet published. We observe a clear change in the overallrotation period distributions over the age range 4-10 Myr, with theprogressively older sub-populations exhibiting systematically faster rotation.This result is consistent with angular momentum evolution model predictions ofan important qualitative change in the stellar rotation periods starting at ~5Myr, an age range for which very few observational constraints were previouslyavailable.

The rotation period distributions of 4--10 Myr T Tauri stars in Orion OB1: New constraints on pre-main-sequence angular momentum evolution