  As the observed occurrence for planets or stellar companions orbiting low and
intermediate-mass evolved stars is increasing, so does the importance of
understanding and evaluating the strength of their interactions. One of the
fundamental mechanisms to understand this interaction is the tidal dissipation
in these stars, as it is one of the engines of orbital/rotational evolution of
star-planet/star-star systems. This article builds on previous works studying
the evolution of the tidal dissipation along the pre-MS and the MS, which have
shown the strong link between the structural and rotational evolution of stars
and tidal dissipation. This article provides for the first time a complete
picture of tidal dissipation along the entire evolution of low and
intermediate-mass stars, including the advanced phases of evolution. Using
stellar evolutionary models, the internal structure of the star is computed
from the pre-MS all the way up to the white dwarf phase, for stars with initial
mass between 1 and 4 Msun. Tidal dissipation is separated into two components:
the dissipation of the equilibrium (non-wavelike) tide and the dissipation of
the dynamical (wavelike) tide. For evolved stars the dynamical tide is
constituted by progressive internal gravity waves. The significance of both the
equilibrium and dynamical tide dissipation becomes apparent within distinct
domains of the parameter space. The dissipation of the equilibrium tide is
dominant when the star is large in size or the companion is far away from the
star. Conversely the dissipation of the dynamical tide is important when the
star is small in size or the companion is close to the star. Both the
equilibrium and the dynamical tides are important in evolved stars, and
therefore both need to be taken into account when studying the tidal
dissipation in evolved stars and the evolution of planetary or/and stellar
companions orbiting them.
