  This investigation is devoted to the effects of nonadiabatic resonant dynamic
tides generated in a uniformly rotating stellar component of a close binary.
The companion is considered to move in a fixed Keplerian orbit, and the effects
of the centrifugal force and the Coriolis force are neglected. Semi-analytical
solutions for the linear, nonadiabatic resonant dynamic tides are derived by
means of a two-time variable expansion procedure. The solution at the lowest
order of approximation consists of the resonantly excited oscillation mode and
displays a phase shift with respect to the tide-generating potential.
Expressions are established for the secular variations of the semi-major axis,
the orbital eccentricity, and the star's angular velocity of rotation caused by
the phase shift. The orders of magnitude of these secular variations are
considerably larger than those derived earlier by Zahn (1977) for the limiting
case of dynamic tides with small frequencies. For a 5 solar mass ZAMS star, an
orbital eccentricity e = 0.5, and orbital periods in the range from 2 to 5
days, numerous resonances of dynamic tides with second-degree lower-order
gravity modes are seen to induce secular variations of the semi-major axis, the
orbital eccentricity, and the star's angular velocity of rotation with time
scales shorter than the star's nuclear life time.
