  One of the most reliable means of studying the stellar interior is through
the apsidal motion in double line eclipsing binary systems since these systems
present errors in masses, radii, and effective temperatures of only a few per
cent. On the other hand, the theoretical values of the apsidal motion to be
compared with the observed values depend on the stellar masses of the
components and more strongly on their radii (fifth power).The main objective of
this work is to make available grids of evolutionary stellar models that, in
addition to the traditional parameters (e.g. age, mass, log g, T$_{\rm eff}$),
also contain the necessary parameters for the theoretical study of apsidal
motion and tidal evolution. This information is useful for the study of the
apsidal motion in eclipsing binaries and their tidal evolution, and can also be
used for the same purpose in exoplanetary systems. All models were computed
using the MESA package. We consider core overshooting for models with masses
$\ge$ 1.2 M$_\odot$. For the amount of core overshooting we adopted a recent
relationship for mass $\times$ core overshooting. We adopted for the
mixing-length parameter $\alpha_{\rm MLT}$ the value 1.84 (the solar-calibrated
value). Mass loss was taken into account in two evolutionary phases. The models
were followed from the pre-main sequence phase to the white dwarf (WD)
stage.The evolutionary models containing age,luminosity, log g, and Teff, as
well as the first three harmonics of the internal stellar structure (k$_2$,
k$_3$, and k$_4$), the radius of gyration $\beta$ y, and the dimensionless
variable $\alpha$, related to gravitational potential energy, are presented in
69 tables covering three chemical compositions: [Fe/H] = -0.50, 0.00, and 0.50.
Additional models with different input physics are available.
