2011MNRAS.416..447S

We investigate the rotational evolution of solar-like stars with a focus on the internal angular momentum transport processes. The double-zone model, in which the star's radiative core and convective envelope are assumed to rotate as solid bodies, is used to test simple relationships between the core–envelope coupling time-scale, τ_c, and rotational properties, like the envelope angular velocity or the differential rotation at the core–envelope interface. The trial relationships are tested by fitting the model parameters to available observations via a Markov chain Monte Carlo method. The synthetic distributions are tested for compatibility with their observational counterparts by means of the standard Kolmogorov–Smirnov (KS) test.

A power-law dependence of τ_c on the inner differential rotation leads to a more satisfactory agreement with observations than a two-valued prescription for τ_c, which would imply a dichotomy between the initially slow (P_rot ≳ 3 d) and fast (P_rot ≲ 3 d) rotators. However, we find it impossible to reconcile the high fraction of fast rotators in α Per with the rotation period distributions in stellar systems at earlier and later evolutionary stages. This could be explained by local environmental effects (e.g. early removal of circumstellar discs due to ultraviolet radiation and winds from nearby high-mass stars) or by observational biases.

The low KS probability that the synthetic and observed distributions are not incompatible, found in some cases, may be due to oversimplified assumptions of the double-zone model, but the large relative uncertainties in the age determination of very young clusters and associations are expected to play a relevant role. Other possible limitations and uncertainties are discussed.