  The tidal interactions of planets affect the stellar evolutionary status and
the constraint of their physical parameters by gyrochronology. In this work, we
incorporate the tidal interaction and magnetic braking of the stellar wind into
MESA and calculate a large grid of 25000 models, covering planets with masses
of 0.1-13.0$\,$$M_{\mathrm{J}}$ with different orbital distances that orbit
late-type stars of different metallicities. We also explore the effect of
different stellar initial rotations on the tidal interactions. Our results show
that in the case of tidal inward migration, the stellar rotation periods are
always lower than that of the star without planet before the planet is engulfed
and the difference in the rotation period of its host star always increases
with time. After the planet is engulfed, the stellar rotation periods are still
lower than that of star without planet, but the difference of periods can be
quickly eliminated if the star has a thick convective envelope(smaller mass and
larger metallicity), regardless of the mass of the planet and the initial
rotation period of the star. In the case of stars with thinner convective
envelopes(larger mass and smaller metallicity), the stars will be spined up and
remain the faster rotation in a long time. Meanwhile, the planet is easily
swallowed and the period differences are large if the initial rotation period
of its host star is higher. Final, we also study the evolution of WASP-19 and
estimate the range of tidal quality parameter $Q'_{*} = (4.6 \pm 0.9) \times
10^{6}$ and initial semi-major axis as $(0.035 \pm 0.004)$$\,$au.
