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(Abbreviated) We extend the results of our 2021 paper concerning the problemof tidal evolution of a binary system with a rotating primary component withrotation axis arbitrarily inclined with respect to the orbital plane. Only thecontribution of quasi-stationary tides is discussed. Unlike previous studies inthis field we present evolution equations derived 'from first principles'. Thegoverning equations contain two groups of terms.  The first group of terms determines the evolution of orbital parameters andinclination angles a 'viscous' time scale. The second group of terms is due tostellar rotation. These terms are present even when dissipation in the star isneglected. Unlike in our 2021 paper we consider all potentially importantsources of apsidal precession in an isolated binary, namely precession arisingfrom the tidal distortion and rotation of the primary as well as Einsteinprecession. We solve these equations numerically for a sample of inputparameters, leaving a complete analysis to an accompanying paper. Periodicchanges to both the inclination of the rotational axis and its precession rateare found. For a particular binary parameters periodic flips between progradeand retrograde rotation are possible. Also, when the inclination angle isallowed to vary, libration of the apsidal angle becomes possible. Furthermore,when the spin angular momentum is larger than the orbital angular momentumthere is a possibility of a significant periodic eccentricity changes.  These phenomena could, in principle, be observed in systems with relativelylarge inclinations and eccentricities such as e.g. those containing a compactobject. In such systems both large inclinations and eccentricities could begenerated as a result of a kick applied to the compact object during asupernova explosion.

Quasi-stationary tidal evolution with arbitrarily misaligned orbital and  stellar angular momenta with a preliminary numerical investigation in the  non-dissipative limit