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We critically examine the constraints on internal angular momentum transportwhich can be inferred from the spin down of open cluster stars. The rotationdistribution inferred from rotation velocities and periods are consistent forlarger and more recent samples, but smaller samples of rotation periods appearbiased relative to vsini studies. We therefore focus on whether the rotationperiod distributions observed in star forming regions can be evolved into theobserved ones in the Pleiades, NGC2516, M34, M35, M37, and M50 with plausibleassumptions about star-disk coupling and angular momentum loss from magnetizedsolar-like winds. Solid body models are consistent with the data for low massfully convective stars but highly inconsistent for higher mass stars where thesurface convection zone can decouple for angular momentum purposes from theradiative interior. The Tayler-Spruit magnetic angular momentum transportmechanism, commonly employed in models of high mass stars, predicts solid-bodyrotation on extremely short timescales and is therefore unlikely to operate insolar-type pre-MS and MS stars at the predicted rate. Models with core-envelopedecoupling can explain the spin down of 1.0 and 0.8 solar mass slow rotatorswith characteristic coupling timescales of 55+-25 Myr and 175+-25 Myrrespectively. The upper envelope of the rotation distribution is more stronglycoupled than the lower envelope of the rotation distribution, in accord withtheoretical predictions that the angular momentum transport timescale should beshorter for more rapidly rotating stars. Constraints imposed by the solarrotation curve are also discussed (Abridged)

Angular Momentum Transport In Solar-Type Stars: Testing the Timescale For Core-Envelope Coupling