  We investigate the long-term dynamical evolution of the internal kinematics
of multimass rotating star clusters. We have performed a set of N-body
simulations to follow the internal evolution of clusters with different degrees
of initial rotation and have explored the evolution of the rotational velocity,
the degree of energy equipartition, and anisotropy in the velocity
distribution. Our simulations show that: 1) as the cluster evolves, the
rotational velocity develops a dependence on the stellar mass with more massive
stars characterised by a more rapid rotation and a peak in the rotation curve
closer to the cluster centre than low-mass stars; 2) the degree of energy
equipartition in the cluster's intermediate and outer regions depends on the
component of the velocity dispersion measured; for more rapidly rotating
clusters, the evolution towards energy equipartition is more rapid in the
direction of the rotational velocity; 3) the anisotropy in the velocity
distribution is stronger for massive stars; 4) both the degree of mass
segregation and energy equipartition are characterised by spatial anisotropy;
they have a dependence on both $R$ and $z$, correlated with the flattening in
the spatial variation of the cluster's density and velocity dispersion, as
shown by 2D maps of the mass segregation and energy equipartition on the
($R$-$z$) meridional plane.
