  The surface angular velocity evolution of low-mass stars is now globally
understood and the main physical mechanisms involved in it are observationally
quite constrained. Additionally, recent observations showed anomalies in the
rotation period distribution of open clusters main sequence early K-type stars
that cannot be reproduced by current angular momentum evolution model. In this
work, we study the parameter space of star-planet system's configurations to
investigate if including the tidal star-planet interaction in angular momentum
evolution models could reproduce these rotation period distribution's
anomalies. To study this effect, we use a parametric angular momentum evolution
model that allows for core-envelope decoupling and angular momentum extraction
by magnetized stellar wind that we coupled to an orbital evolution code where
we take into account the torque due to the tides raised on the star by the
planet. We explore different stellar and planetary configurations (stellar mass
from 0.5 to 1.0 $\rm M_{\odot}$ and planetary mass from 10 $\rm M_{\oplus}$ to
13 $\rm M_{\rm jup}$) to study their effect on the planetary orbital and
stellar rotational evolution. The stellar angular momentum is the most impacted
by the star-planet interaction when the planet is engulfed during the early
main sequence phase. Thus, if a close-in Jupiter mass planet is initially
located around 50\% of the stellar corotation radius, a kink in the rotational
period distribution opens around late and early K-type stars during the early
main sequence phase. Tidal star-planet interactions can create a kink in the
rotation period distribution of low-mass stars, which could possibly account
for unexpected scatter seen in the rotational period distribution of young
stellar clusters.
