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The braking of main sequence stars originates mainly from their stellar wind.The efficiency of this angular momentum extraction depends on the rotation rateof the star, the acceleration profile of the wind and the coronal magneticfield. The derivation of scaling laws parametrizing the stellar wind torque isimportant for our understanding of gyro-chronology and the evolution of therotation rates of stars. In order to understand the impact of complex magnetictopologies on the stellar wind torque, we present three- dimensional, dynamicalsimulations of the corona of HD 189733. Using the observed complex topology ofthe magnetic field, we estimate how the torque associated with the wind scaleswith model parameters and compare those trends to previously published scalinglaws.

Modelling the Corona of HD 189733 in 3D