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 for the limiting case of dynamic tides with small frequencies .
For a 5 M _ { \odot } 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 g ^ { + } -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 .