Effect of Differential Rotation on the Magnetic Braking of Low-mass and Solar-like Stars: A Proof-of-concept Study

On the main sequence, low-mass and solar-like stars are observed to spin-down over time, magnetized stellar winds thought be predominantly responsible for this significant angular momentum loss. Previous studies have demonstrated that wind torque can predicted via formulations dependent on properties, such as magnetic field strength geometry, radius mass, mass-loss rate, rotation rate. Although these experience surface differential rotation, so far assumed solid-body rotation. Surface is expected affect of thus To investigate how affects torque, we use PLUTO code perform 2.5D magnetohydrodynamic, axisymmetric simulations winds, using a colatitude-dependent profile (i.e., slower at poles than equator). We demonstrate determined by average rate in wind, net less assuming equatorial The magnitude effect essentially proportional example, resulting Sun $\sim 20 \%$ smaller assumption. derive fit semi-analytic formulation predicts function spin magnetization (depending dipolar combined).