  Unraveling the internal kinematics of open clusters is crucial for
understanding their formation and evolution. However, there is a dearth of
research on this topic, primarily due to the lack of high-quality kinematic
data. Using the exquisite-precision astrometric parameters and radial
velocities provided by Gaia data release 3, we investigate the internal
rotation in three of the most nearby and best-studied open clusters, namely the
Pleiades, Alpha Persei, and Hyades clusters. Statistical analyses of the
residual motions of the member stars clearly indicate the presence of
three-dimensional rotation in the three clusters. The mean rotation velocities
of the Pleiades, Alpha Persei, and Hyades clusters within their tidal radii are
estimated to be 0.24 (0.04), 0.43 (0.08), and 0.09 (0.03) km s-1, respectively.
Similar to the Praesepe cluster that we have studied before, the rotation of
the member stars within the tidal radii of these three open clusters can be
well interpreted by Newton's theorem. No expansion or contraction is detected
in the three clusters either. Furthermore, we find that the mean rotation
velocity of open clusters may be positively correlated with the cluster mass,
and the rotation is likely to diminish as open clusters age.
