  Although a large number of Galactic open clusters (OCs) have been identified,
the internal kinematic properties (e.g., rotation) of almost all the known OCs
are still far from clear. With the high-precision astrometric data of Gaia
EDR3, we have developed a methodology to unveil the rotational properties of
the Praesepe cluster. Statistics of the three-dimensional residual motions of
the member stars reveal the presence of Praesepe's rotation and determine its
spatial rotation axis. The mean rotation velocity of the Praesepe cluster
within its tidal radius is estimated to be 0.2 $\pm$ 0.05 km s$^{-1}$, and the
corresponding rotation axis is tilted in relation to the Galactic plane with an
angle of 41 $\pm$ 12 degree. We also analysed the rms rotational velocity of
the member stars around the rotation axis, and found that the rotation of the
member stars within the tidal radius of Praesepe probably follows the Newton's
classical theorems.
