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Aims: We study the evolution of stellar rotation and wind properties forlow-mass main-sequence stars. Our aim is to use rotational evolution models toconstrain the mass loss rates in stellar winds and to predict how theirproperties evolve with time on the main-sequence.  Methods: We construct a rotational evolution model that is driven by observedrotational distributions of young stellar clusters. Fitting the free parametersin our model allows us to predict how wind mass loss rate depends on stellarmass, radius, and rotation. We couple the results to the wind model developedin Paper I of this series to predict how wind properties evolve on themain-sequence.  Results: We estimate that wind mass loss rate scales with stellar parametersas $\dot{M}_\star \propto R_\star^2 \Omega_\star^{1.33} M_\star^{-3.36}$. Weestimate that at young ages, the solar wind likely had a mass loss rate that isan order of magnitude higher than that of the current solar wind. This leads tothe wind having a higher density at younger ages; however, the magnitude ofthis change depends strongly on how we scale wind temperature. Due to thespread in rotation rates, young stars show a large range of wind properties ata given age. This spread in wind properties disappears as the stars age.  Conclusions: There is a large uncertainty in our knowledge of the evolutionof stellar winds on the main-sequence, due both to our lack of knowledge ofstellar winds and the large spread in rotation rates at young ages. Given thesensitivity of planetary atmospheres to stellar wind and radiation conditions,these uncertainties can be significant for our understanding of the evolutionof planetary environments.

Stellar Winds on the Main-Sequence II: the Evolution of Rotation and Winds