  We determine the response of a uniformly rotating star to tidal perturbations
due to a companion. General periodic orbits and parabolic flybys are
considered. We evaluate energy and angular momentum exchange rates as a sum of
contributions from normal modes allowing for dissipative processes. We consider
the case when the response is dominated by the contribution of an identifiable
regular spectrum of low frequency modes, such as gravity modes and evaluate it
in the limit of very weak dissipation. Our formalism may be applied both to
Sun-like stars with radiative cores and convective envelopes and to more
massive stars with convective cores and radiative envelopes. We provide general
expressions for transfer of energy and angular momentum valid for an orbit with
any eccentricity.
  Detailed calculations are made for Sun-like stars in the slow rotation regime
where centrifugal distortion is neglected in the equilibrium and the
traditional approximation is made for the normal modes. We use both a WKBJ
procedure and direct numerical evaluation which are found to be in good
agreement for regimes of interest.
  Finally we use our formalism to determine the evolution time scales for an
object, in an orbit of small eccentricity, around a Sun-like star in which the
tidal response is assumed to occur. Systems with either no rotation or
synchronous rotation are considered. Only rotationally modified gravity modes
are taken into account under the assumption that wave dissipation occurs close
to the stellar centre.
