  Stellar winds govern the spin-down of Solar-type stars as they age, and play
an important role in determining planetary habitability, as powerful winds can
lead to atmospheric erosion. We calculate three-dimensional stellar wind models
for five young Solar-type stars in the Hyades cluster, using TOUPIES survey
stellar magnetograms and state-of-the-art Alfv\'en wave driven wind modelling.
The stars have the same 0.6-Gyr age and similar fundamental parameters, and we
account for the uncertainty in and underestimation of absolute field strength
inherent in Zeeman-Doppler imaging by adopting both unscaled and scaled (by a
factor of five) field strengths. For the unscaled fields, the resulting stellar
wind mass loss is 2-4 times greater and the angular momentum loss 2-10 times
greater than for the Sun today, with the scaled results correspondingly
greater. We compare our results with a range published of wind models and for
the Alfv\'en wave driven modelling see evidence of mass loss saturation at
about $10 \dot M_\odot$.
