  Solar-type stars, which shed angular momentum via magnetised stellar winds,
enter the main sequence with a wide range of rotational periods $P_\text{rot}$.
This initially wide range of rotational periods contracts and has mostly
vanished by a stellar age $t\sim0.6$ Gyr, after which Solar-type stars spin
according to the Skumanich relation $P_\text{rot}\propto\sqrt t$.
Magnetohydrodynamic stellar wind models can improve our understanding of this
convergence of rotation periods. We present wind models of fifteen young
Solar-type stars aged from 24 Myr to 0.13 Gyr. With our previous wind models of
stars aged 0.26 Gyr and 0.6 Gyr we obtain thirty consistent three-dimensional
wind models of stars mapped with Zeeman-Doppler imaging - the largest such set
to date. The models provide good cover of the pre-Skumanich phase of stellar
spin-down in terms of rotation, magnetic field, and age. We find that the mass
loss rate $\dot M\propto\Phi^{0.9\pm0.1}$ with a residual spread of 150% and
that the wind angular momentum loss rate $\dot J\propto{}P_\text{rot}^{-1}
\Phi^{1.3\pm0.2}$ with a residual spread of 500% where $\Phi$ is the unsigned
surface magnetic flux. When comparing different magnetic field scalings for
each single star we find a gradual reduction in the power-law exponent with
increasing magnetic field strength.
