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We developed angular momentum evolution models for 0.5 and 0.8 $M_{\odot}$stars. The parametric models include a new wind braking law based on recentnumerical simulations of magnetised stellar winds, specific dynamo andmass-loss rate prescriptions, as well as core/envelope decoupling. We comparemodel predictions to the distributions of rotational periods measured for lowmass stars belonging to star forming regions and young open clusters.Furthermore, we explore the mass dependence of model parameters by comparingthese new models to the solar-mass models we developed earlier. Rotationalevolution models are computed for slow, median, and fast rotators at eachstellar mass. The models reproduce reasonably well the rotational behaviour oflow-mass stars between 1 Myr and 8-10 Gyr, including pre-main sequence tozero-age main sequence spin up, prompt zero-age main sequence spin down, andearly-main sequence convergence of the surface rotation rates. Fast rotatorsare found to have systematically shorter disk lifetimes than moderate and slowrotators, thus enabling dramatic pre-main sequence spin up. They also haveshorter core-envelope coupling timescales, i.e., more uniform internalrotation. As to the mass dependence, lower mass stars require significantlylonger core-envelope coupling timescale than solar-type ones, which results instrong differential rotation developing in the stellar interior on the earlymain sequence. Lower mass stars also require a weaker braking torque to accountfor their longer spin down timescale on the early main sequence, while theyultimately converge towards lower rotational velocities than solar-type starson the longer term due to their reduced moment of inertia. We also findevidence that the mass-dependence of the wind braking efficiency may be relatedto a change of the magnetic topology in lower mass stars.

Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence