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tokens: higher rotational velocities than expected for single stars, we conclude that stellar multiplicity is an important enhancer of rotation in Sun-like stars. Blue stragglers are expected to have a strong enhancement on rotation owing to injection of angular momentum from the donor companion. 5. The rotational braking law We removed from this analysis all the spectroscopic binaries in order to correctly constrain the rotational braking. The non-SB HIP 29525 displays a that is much higher than expected ( km s), but it is likely that this is the result of an overestimated isochronal age ( Gyr). We decided to not include HIP 29525 in the rotational braking determination because it is a clear outlier in our results. Maldonado et al. (2010) found X-ray and chromospheric ages of 0.55 and 0.17 Gyr, respectively, for HIP 29525. We then divided the remaining 65 stars and the Sun in bins of 2 Gyr, and removed all the stars that were below the 70th percentile of in each bin from this sample. Such a procedure can be justified because we verified that 30% of the stars should have above 0.9 by doing a simple simulation with angles drawn from a flat distribution between 0 and . This allowed us to select the stars that had the highest chance of having above . In total, 21 solar twins and the Sun compose what we hereafter reference as the selected sample . Albeit this subsample is smaller, it has the advantage of mostly removing uncertainties on the inclination angle of the stellar rotation axes 7 . We stress that the only reason we can select the most probable edge-on rotating stars () is because we have a large sample of solar twins in the first place. We then proceeded to fit a general curve to the selected sample (see Fig. 5 ) using the method of orthogonal distance regression (ODR, Boggs Rogers 1990 ), which takes the uncertainties on both and ages into account. This curve is a power law plus constant of the form (the same chromospheric activity and vs. age relation used by Pace Pasquini 2004 ; Guinan Engle 2009 ), with (rotational velocity) and (asymptotic velocity) in km s and (age) in Gyr. We find that the best-fit parameters are , , and (see right panel of Fig. 5 ). These large uncertainties are likely due to i) the strong correlation between and ; and ii) the relatively limited number of data points between 1 and 4 Gyr, where the parameters are most effective in changing the values of . This limitation is also present in past studies (e.g., van Saders et al. 2016 ; Barnes 2003 ; Pace Pasquini 2004 ; Mamajek Hillenbrand 2008 ; García et al. 2014 ; Amard et al. 2016 ). On the other hand, our sample is the largest comprising solar twins and, therefore, should produce more reliable results. With more data points, we could be able to use 1 Gyr bins instead of 2 Gyr in order to select the fastest rotating stars, which would result in a better subsample for constraining the rotational evolution for young stars. The relation we obtain is in contrast with some