  The detection of oscillations with a mixed character in subgiants and red
giants allows us to probe the physical conditions in their cores. With these
mixed modes, we aim at determining seismic markers of stellar evolution. Kepler
asteroseismic data were selected to map various evolutionary stages and stellar
masses. Seismic evolutionary tracks were then drawn with the combination of the
frequency and period spacings. We measured the asymptotic period spacing for
more than 1170 stars at various evolutionary stages. This allows us to monitor
stellar evolution from the main sequence to the asymptotic giant branch and
draw seismic evolutionary tracks. We present clear quantified asteroseismic
definitions that characterize the change in the evolutionary stages, in
particular the transition from the subgiant stage to the early red giant
branch, and the end of the horizontal branch.The seismic information is so
precise that clear conclusions can be drawn independently of evolution models.
The quantitative seismic information can now be used for stellar modeling,
especially for studying the energy transport in the helium-burning core or for
specifying the inner properties of stars entering the red or asymptotic giant
branches. Modeling will also allow us to study stars that are identified to be
in the helium-subflash stage, high-mass stars either arriving or quitting the
secondary clump, or stars that could be in the blue-loop stage.
