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Young and rapidly rotating stars are known for intense, dynamo generatedmagnetic fields. Spectropolarimetric observations of those stars in preciselyaged clusters are key input for gyrochronology and magnetochronology. We useZDI maps of several young K-type stars of similar mass and radius but withvarious ages and rotational periods, to perform 3D numerical MHD simulations oftheir coronae and follow the evolution of their magnetic properties with age.Those simulations yield the coronal structure as well as the instant torqueexerted by the magnetized, rotating wind on the star. As stars get older, wefind that the angular momentum loss decreases with $\Omega^3$, which is thereason for the convergence on the Skumanich law. For the youngest stars of oursample, the angular momentum loss show signs of saturation around$8\Omega_{\odot}$, which is a common value used in spin evolution models forK-type stars. We compare these results to semi-analytical models and existingbraking laws. We observe a complex wind speed distribution for the youngeststars with slow, intermediate and fast wind components, which are the result ofthe interaction with intense and non axisymmetric magnetic fields.Consequently, in our simulations, the stellar wind structure in the equatorialplane of young stars varies significantly from a solar configuration,delivering insight about the past of the solar system interplanetary medium.

Age dependence of wind properties for solar type stars: a 3d study