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S. A. Barnes (Lowell observatory), S. Sofia (Yale University)
Newly obtained data have significantly expanded the rotation period database for solar-type stars (1.2-0.6 solar mass) in young open clusters. This warrants a comparison with recent models of stellar angular momentum evolution. We present such a comparison, including the mass-dependence of stellar rotation, with emphasis on the phenomena of magnetic saturation and disk-star interaction on the pre-main sequence. The `best' models suggest disk lifetimes of the order of 1 to a few Myr on the pre-main sequence.