  While the number of detected planets is continuously increasing since 1995,
their impact on their central star still remain poorly understood. Yet, the
presence of a massive close-in planet can strongly modify the surface angular
velocity evolution of the star. In these circumstances, age estimation
techniques based on rotation, such as the gyrochronology, can't be applied to
stars that experienced significant star-planet magnetic and tidal interactions
during their evolution. With the use of a numerical model that combines an
angular momentum evolution and an orbital evolution code, we investigated the
evolution of initial distribution of star-planet systems, in which the orbital
evolution of the planet is driven by the tidal dissipation formalism. Based on
these initial distributions we highlighted the limits of applicability of the
gyrochronology analysis and proposed a new age determination technique based on
the observation of the couple $\rm P_{rot,\star}$-$a$, where $\rm
P_{rot,\star}$ is the stellar rotational period and $a$ the planetary
semi-major axis. This technique called tidal-chronology can be very helpful for
planetary system composed of a star between 0.3 and 1.2 $\rm M_{\odot}$ and a
planet more massive than 1 $\rm M_{jup}$ initially located at few hundredth au
of the host star.
