  (Abbreviated) We extend the results of our 2021 paper concerning the problem
of tidal evolution of a binary system with a rotating primary component with
rotation axis arbitrarily inclined with respect to the orbital plane. Only the
contribution of quasi-stationary tides is discussed. Unlike previous studies in
this field we present evolution equations derived 'from first principles'. The
governing equations contain two groups of terms.
  The first group of terms determines the evolution of orbital parameters and
inclination angles a 'viscous' time scale. The second group of terms is due to
stellar rotation. These terms are present even when dissipation in the star is
neglected. Unlike in our 2021 paper we consider all potentially important
sources of apsidal precession in an isolated binary, namely precession arising
from the tidal distortion and rotation of the primary as well as Einstein
precession. We solve these equations numerically for a sample of input
parameters, leaving a complete analysis to an accompanying paper. Periodic
changes to both the inclination of the rotational axis and its precession rate
are found. For a particular binary parameters periodic flips between prograde
and retrograde rotation are possible. Also, when the inclination angle is
allowed to vary, libration of the apsidal angle becomes possible. Furthermore,
when the spin angular momentum is larger than the orbital angular momentum
there is a possibility of a significant periodic eccentricity changes.
  These phenomena could, in principle, be observed in systems with relatively
large inclinations and eccentricities such as e.g. those containing a compact
object. In such systems both large inclinations and eccentricities could be
generated as a result of a kick applied to the compact object during a
supernova explosion.
