  TZ Fornacis is a double-lined eclipsing binary system with similar masses
(2.057$\pm$0.001 and 1.958$\pm$0.001 $M_{\odot}$) but characterized by very
different radii (8.28$\pm$0.22 and 3.94$\pm$0.17 $R_{\odot}$). This similarity
in terms of mass makes it possible to study the system's differential stellar
evolution as well as some aspects of its tidal evolution. With regard to its
orbital elements, it was recently confirmed that its orbit is circular with an
orbital period of 75.7 days. The less massive component rotates about 17 times
faster than the primary one, which is synchronized with the mean orbital
angular velocity. Our main objective in this work is to study both the nuclear
and the tidal evolution of the system. We explored two scenarios regarding the
initial eccentricities: a high one (0.30) and a case of an initial circular
orbit. A good agreement has been found between the observational values of the
eccentricity, synchronism levels, and orbital period with the values predicted
by the integration of the tidal evolution equations. The influence of the
friction timescale on the evolution of the orbital elements of TZ For is also
studied here. The orbital elements most affected by the uncertainties in the
friction timescale are the synchronism levels of the two components. On the
other hand, we used the properties of the rotating models generated by the
GRANADA code as the initial angular velocities instead of using trial values.
In this case, comparisons between the theoretical values of the orbital
elements and their observed counterparts also lead to a good interagreement.
