  We propose a novel method to constrain the tidal quality factor, $Q'$, from
an observed non-synchronized star-planet system consisting of a slowly rotating
low-mass star and a close-in Jovian planet, taking into account the
co-evolution of stellar spin and planetary orbit due to the tidal interaction
and the magnetic braking. On the basis of dynamical system theory, the track of
the co-evolution of angular momentum from the fast rotator regime for such a
system exhibits the existence of a forbidden region in the
$\Omega_\mathrm{orb}$ -- $\Omega_\mathrm{spin}$ plane , where
$\Omega_\mathrm{spin}$ and $\Omega_\mathrm{orb}$ denote the angular velocity of
the stellar spin and planetary orbit, respectively. The forbidden region is
determined primarily by the strength of the tidal interaction. By comparing
($\Omega_\mathrm{orb},\Omega_\mathrm{spin}$) of a single star-planet system to
the forbidden region, we can constrain the tidal quality factor regardless of
the evolutionary history of the system. The application of this method to the
star-planet system, NGTS-10 -- NGTS-10 b, gives $Q' \gtrsim 10^8$, leading to
an tight upper bound on the tidal torque. Since this cannot be explained by
previous theoretical predictions for non-synchronized star-planet systems, our
result requires mechanisms that suppress the tidal interaction in such systems.
