Evolution of the slow and fast wind speeds at 1 AU for different stellar masses assuming Model A for determining the wind temperature. In this model, we assume that the wind temperature can be scaled with the coronal temperature. We calculate the wind speed at 1 AU using Eq. (19). The three panels correspond to different ages, and in each panel, the lower and upper lines correspond to the wind speeds for stars at the 10th and 90th percentiles of the rotational distributions respectively. In the case of the low-mass stars in the upper panel, there is only one line because both percentiles lie above the saturation threshold, and therefore have the same wind temperatures. The lower and upper dashed black lines show the Michel velocity along the 10th and 90th percentile tracks, which is an estimate of the terminal wind speed in the equatorial plane due to magneto-rotational acceleration, as discussed in Sect. 6.1.