  When planets are formed from the protoplanetary disk and after the disk has
dissipated, the evolution of their orbits is governed by tidal interactions,
friction, and gravitational drag, and also by changes in the mass of the star
and planet. These interactions may change the initial distribution of the
distances between the planets and their host star by expanding the original
orbit, by contracting it (which may cause an engulfment of the planet by the
star), or by destroying the planet. We study the evolution of the orbit of a
planet orbiting its host star under the effects of equilibrium tides, dynamical
tides, drag (frictional and gravitational), and stellar mass loss. We used the
Geneva stellar evolution code to compute the evolution of stars with initial
masses of 1 and 1.5 solar mass with different rotation rates at solar
metallicity. The star is evolved from the pre-main-sequence (PMS) up to the tip
of the red giant branch. We used these models as input for computing the
evolution of the planetary orbits. We explored the effects of changing the
planet masses (of 1 Earth mass up to 20 Jupiter masses), the distance between
the planet and the star (of 0.015 and more than 3 au), the mass, and the spin
of the star. We present results when only the equilibrium tide was accounted
for and when both equilibrium and dynamical tides were accounted for. The
expression for the dynamical tide is a frequency-averaged dissipation of
tidally excited inertial waves, obtained from a piecewise homogeneous two-layer
stellar model. Gravity wave damping was neglected. Dynamical tides in
convective zones have a significant effect on planetary orbits only during the
PMS phase and only for fast-rotating stars. They have no significant effects
during the PMS phase for initially slow-rotating stars and during the red giant
branch phase, regardless of the initial rotation (abridged).
