  Splaver and coworkers have measured the masses of the white dwarf and the
neutron star components of the PSR J1713+0747 binary system pair by Shapiro
Delay. We attempt to find the original configuration of this system performing
a set of binary evolution calculations to simultaneously account for the masses
of both stars and the orbital period. We considered initial masses of 1.5 and
1.4 \msun for the normal (donor) and the neutron star, respectively. We assumed
two metallicity values (Z = 0.010 and 0.020), and an initial orbital period
near 3 days. We assume that the neutron star is only able to retain \lesssim
0.10 of the matter transferred by the donor star.
  Calculations were performed employing our binary hydro code that handles the
mass transfer rate in a fully implicit way together with state-of-the-art
physical ingredients, diffusion and a non-grey atmospheres.
  We compare the structure of the resulting white dwarfs with the
characteristic age of PSR J1713+0747 finding a nice agreement with observations
by Lundgren et al. especially for the case of a donor star with Z= 0.010. This
result indicates that the evolution of this kind of binary system is well
understood.
  The models predict that, due to diffusion, the atmosphere of the white dwarf
is an almost hydrogen-pure one. We find that such structures are unable to
account for the colours measured by Lundgren et al. within their error bars.
Thus, some discrepances in the white dwarf emergent radiation remain to be
explained.
