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