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This investigation is devoted to the effects of nonadiabatic resonant dynamictides generated in a uniformly rotating stellar component of a close binary.The companion is considered to move in a fixed Keplerian orbit, and the effectsof the centrifugal force and the Coriolis force are neglected. Semi-analyticalsolutions for the linear, nonadiabatic resonant dynamic tides are derived bymeans of a two-time variable expansion procedure. The solution at the lowestorder of approximation consists of the resonantly excited oscillation mode anddisplays 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 bythe phase shift. The orders of magnitude of these secular variations areconsiderably larger than those derived earlier by Zahn (1977) for the limitingcase of dynamic tides with small frequencies. For a 5 solar mass ZAMS star, anorbital eccentricity e = 0.5, and orbital periods in the range from 2 to 5days, numerous resonances of dynamic tides with second-degree lower-ordergravity modes are seen to induce secular variations of the semi-major axis, theorbital eccentricity, and the star's angular velocity of rotation with timescales shorter than the star's nuclear life time.Comment: accepted for publication in A&A, 13 page

Nonadiabatic resonant dynamic tides and orbital evolution in close binaries