Slow-rotator sequence radii

Here it is applied for the first time to the dataset available for the Pleiades. We find an agreement better than ~10 percent between the observed R vs M_K_ relationship and current standard stellar models for 1.2>=M/M_{sun}_>=0.85 with no evident bias. Evidence of a systematic deviation at 2sigma level are found for stars with 0.8>=M/M_{sun}_=0.6 approaching the slow-rotator sequence.

Fast-rotators (P<2d) agree with standard models within 15 percent with no systematic deviations in the whole 1.2>=M/M_{sun}_>=0.5 range. The evidence found of a possible radius inflation just below the lower mass limit of the slow-rotator sequence indicates a possible connection with the transition from the fast to the slow-rotator sequence.