  The stellar rotation has an essential role in modifying the structure of the
star and, therefore, the way these different interplays arise. On the other
hand, changes in orbits impact the star's rotation and its evolution. The
evolution of the star's rotation accounts for the angular momentum exchange
with the planet and follows the effects of the internal transport of angular
momentum and metallicity. Several models in the literature have aimed to find a
theoretical way to study these interactions between the planet's orbital
evolution and the star's rotation. Our work is a promising attempt to
investigate these interactions from a model based on a new statistical
approach. To this end, we propose a ``tidal interaction index'' that carries
all the parameters of the star-planet system that can affect the transport of
angular momentum and, consequently, the evolution of stellar rotation. This
index is similar to the ``magnetic braking index'' whose most successful value
equals 3, which expresses the seminal Skumunich law. Our model is computed for
masses of the host star less than the Kraft limit for three orbital-rotation
period regimes and the semi-major axis less than 1 AU. We consider planets with
masses between 0.4M$_{\oplus}$ and 20M$_{\rm J}$ with orbital periods between
0.3 and 225 days. We show that the tidal index $q$ segregated by stellar mass
without wind magnetic braking during the main-sequence phase is strongly
anti-correlated with planetary mass. Finally, we conclude that in cases where
planets retain less than 84\% of the total angular momentum within the system,
the magnetic braking mechanism proves to be more effective than tidal
interactions, irrespective of whether the planets' angular momentum surpasses
that of the host star.
