  [Abridged] Most exoplanets detected so far are close-in planets, which are
likely to be affected by tidal dissipation in their host star. To get a
complete picture of the evolution of star-planet systems one needs to consider
the impact of tides within both stellar radiative and convective zones. We aim
to provide a general formalism to assess tidal dissipation in stellar radiative
zones for all spectral types, allowing for the study of the dynamics of a given
system throughout stellar evolution. We investigate the influence of stellar
structure and evolution on tidal dissipation in the radiative core of low-mass
stars. From the study of adiabatic oscillations throughout the star, we compute
the energy flux transported by progressive internal gravity waves and the
induced tidal torque. We then study the influence of stellar structure and
evolution on tidal dissipation of solar-type stars from the pre-main sequence
(PMS) to the red giant branch (RGB). For a given star-planet system, tidal
dissipation reaches a maximum value on the pre-main sequence for all stellar
masses. On the main sequence (MS), it decreases to become almost constant. The
dissipation is then several orders of magnitude smaller for F-type stars than
for G and K-type stars. During the Sub-Giant phase and the RGB, tidal
dissipation increases by several orders of magnitude, along with the expansion
of the stellar envelope. We show that the dissipation of the dynamical tide in
the convective zone dominates the evolution of the system during most of the
PMS and the beginning of the main sequence. Tidal dissipation in the radiative
zone then becomes the strongest contribution during the Sub-Giant phase and the
RGB. We also find that the dissipation of a metal-poor star is stronger than
the dissipation of a metal-rich star during the PMS, the Sub-Giant phase and
the RGB.
