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