  Age estimation techniques such as gyrochronology and magnetochronology can't
be applied to stars that exchanged angular momentum with their close
environment. This is especially true for massive close-in planetary companion
(with a periods of few days or less), which could have been strongly impacted
the rotational evolution of the host star, along the stellar evolution, through
the star-planet tidal interaction.
  We showed that the interaction of a close-in massive planet with its host
star can strongly modify the surface rotation rate of this latter, in most of
the cases associated to a planetary engulfment. In such cases, a gyrochronology
analysis of the star would wrongly make it appear as "rejuvenated", thus
preventing us to use this method with confidence. To try overcome this issue,
we eventually proposed the proof of concept of a new age determination
technique that we call the tidal-chronology, which is based on the observed
couple $\rm P_{rot,\star}$-$\rm P_{orb}$ of a given star-planet system.
  The gyrochronology technique can only be applied to isolated star or
star-planet systems outside a specific range of $\rm P_{rot,\star}$-$\rm
P_{orb}$. This region tends to expand for increasing stellar and planetary
mass. In that forbidden region, or if any planetary engulfment is suspected,
gyrochronology should be used with extreme caution while tidal-chronology could
be considered. While this technique does not provide a precise age for the
system yet, it is already an extension of gyrochronology and could be helpful
to determine a more precise range of possible age for planetary system composed
of a star between 0.3 and 1.2 $M_{\odot}$ and a planet more massive than 1 $\rm
M_{jup}$ initially located at few hundredth au of the host star.
