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We present the results of a multi-filter photometric monitoring of the widebinary HIP10680/HIP10679. We found both component to be variable with amplitudeup to $\Delta$V = 0.03 mag in the case of HIP10680 and $\Delta$V = 0.07 mag inthe case of HIP10679. We could measure the rotation periods P = 0.2396d of thehotter F5V component HIP10680 and P = 0.777d of the cooler G5V componentHIP10679. We found that the rotation axes of both components are aligned withan inclination $i$ = $\sim$ 10$^{\circ}$. Although the two components have amass difference not larger than 15%, they exhibit a significant differencebetween their rotation periods. Such difference may arise either from differentinitial rotation periods or to different disc life times. For instance, theslower rotating component HIP 10679 hosts a well know debris disc.

HIP10680/HIP10679: a visual binary in the $\beta$ Pictoris Association with the fastest rotating member