  Our aim is to investigate the tidal interaction in High-mass X-ray Binaries
and Symbiotic stars in order to determine in which objects the rotation of the
mass donors is synchronized or pseudosynchronized with the orbital motion of
the compact companion. We find that the Be/X-ray binaries are not synchronized
and the orbital periods of the systems are greater than the rotational periods
of the mass donors. The giant and supergiant High-mass X-ray binaries and
symbiotic stars are close to synchronization. We compare the rotation of mass
donors in symbiotics with the projected rotational velocities of field giants
and find that the M giants in S-type symbiotics rotate on average 1.5 times
faster than the field M giants. We find that the projected rotational velocity
of the red giant in symbiotic star MWC 560 is v sin i = 8.2 +/- 1.5 km/s, and
estimate its rotational period to be Prot = 144 - 306 days. Using the
theoretical predictions of tidal interaction and pseudosynchronization, we
estimate the orbital eccentricity e = 0.68 - 0.82.
