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 \pm 1.5 km s ^ { - 1 } , and estimate its rotational period to be P _ { rot } = 144 - 306 days . Using the theoretical predictions of tidal interaction and pseudosynchronization , we estimate the orbital eccentricity e = 0.68 - 0.82 .