  Star-disk interaction is thought to drive the angular momentum evolution of
young stars. In this review, I present the latest results obtained on the
rotational properties of low mass and very low mass pre-main sequence stars. I
discuss the evidence for extremely efficient angular momentum removal over the
first few Myr of pre-main sequence evolution and describe recent results that
support an accretion-driven braking mechanism. Angular momentum evolution
models are presented and their implication for accretion disk lifetimes
discussed.
