  The present work is based on a description for the angular mometum loss rate
due to magnetic braking for main-sequence stars on the relationship between
stellar rotation and age. In general, this loss rate denoted by $\mathrm
dJ/\mathrm dt$ depends on angular velocity $\Omega$ in the form $\mathrm
dJ/\mathrm dt\propto\Omega^{q}$, where $q$ is a parameter extracted from
nonextensive statistical mechanics. Already, in context of stellar rotation,
this parameter is greater than unity and it is directly related to the braking
index. For $q$ equal to unity, the scenario of saturation of the magnetic field
is recovered, otherwise $q$ indicates an unsaturated field. This new approach
have been proposed and investigated by de Freitas \& De Medeiros for
unsaturated field stars. In present work, we propose a nonextensive approach
for the stellar rotational evolution based on the Reiners \& Mohanthy model. In
this sense, we developed a nonextensive version of Reiners \& Mohanthy torque
and also compare this generalized version with the model proposed in de Freitas
\& De Medeiros based on the spin-down Kawaler torque for the main-sequence
stars with F and G spectral types. We use the same sample of $\sim16 000$ field
stars with rotational velocity $v \sin i$ limited in age and mass. As a result,
we show that the Kawaler and Reiners \& Mohanthy models exhibit strong
discrepancies, mainly in relation to the domain of validity of the entropic
index $q$. These discrepancies are mainly due to sensitivity on the stellar
radius. Finally, our results showed that modified Kawaler prescription is
compatible with a wider mass range, while the Reiners \& Mohanty model is
restricted to masses less than G6 stars.
