  Time-dependent nonextensivity in a stellar astrophysical scenario combines
nonextensive entropic indices $q_{K}$ derived from the modified Kawaler's
parametrization, and $q$, obtained from rotational velocity distribution. These
$q$'s are related through a heuristic single relation given by $q\approx
q_{0}(1-\Delta t/q_{K})$, where $t$ is the cluster age. In a nonextensive
scenario, these indices are quantities that measure the degree of
nonextensivity present in the system. Recent studies reveal that the index $q$
is correlated to the formation rate of high-energy tails present in the
distribution of rotation velocity. On the other hand, the index $q_{K}$ is
determined by the stellar rotation-age relationship. This depends on the
magnetic field configuration through the expression $q_{K}=1+4aN/3$, where $a$
and $N$ denote the saturation level of the star magnetic field and its
topology, respectively. In the present study, we show that the connection
$q-q_{K}$ is also consistent with 548 rotation period data for single
main-sequence stars in 11 Open Clusters aged less than 1 Gyr. The value of
$q_{K}\sim$ 2.5 from our unsaturated model shows that the mean magnetic field
topology of these stars is slightly more complex than a purely radial field.
Our results also suggest that stellar rotational braking behavior affects the
degree of anti-correlation between $q$ and cluster age $t$. Finally, we suggest
that stellar magnetic braking can be scaled by the entropic index $q$.
