2020ApJ...896..123S

Observations of stellar rotation show that low-mass stars lose angular momentum during the main sequence. We simulate the winds of sunlike stars with a range of rotation rates, covering the fast and slow magneto-rotator regimes, including the transition between the two. We generalize an Alfven-wave-driven solar wind model that builds on previous works by including the magneto-centrifugal force explicitly. In this model, the surface-averaged open magnetic flux is assumed to scale as B_*f_*^open∝Ro^–1.2, where f_*^open and Ro are the surface open-flux filling factor and Rossby number, respectively. We find that, (1) the angular-momentum loss rate (torque) of the wind is described as τ_w~2.59×10³⁰ erg (Ω_*/Ω_☉)^2.82, yielding a spin-down law Ω_*∝t^–0.55. (2) The mass-loss rate saturates at {dot}M_w∼3.4×10^–14M_☉ yr^–1, due to the strong reflection and dissipation of Alfven waves in the chromosphere. This indicates that the chromosphere has a strong impact in connecting the stellar surface and stellar wind. Meanwhile, the wind ram pressure scales as P_w∝Ω_*^0.57, which is able to explain the lower envelope of the observed stellar winds by Wood et al. (3) The location of the Alfven radius is shown to scale in a way that is consistent with one-dimensional analytic theory. Additionally, the precise scaling of the Alfven radius matches previous works, which used thermally driven winds. Our results suggest that the Alfven-wave-driven magnetic rotator wind plays a dominant role in the stellar spin-down during the main sequence.