  V404 Cyg is a Low Mass X-Ray Binary (LMXB) system that has undergone
outbursts in 1938, 1989, and 2015. During these events, it has been possible to
determine relevant data of the system; such as the masses of the compact object
(a black hole, BH) and its companion, the orbital period, the companion
spectral type, and luminosity class, among others. Remarkably, the companion
star has a metallicity appreciably higher than solar. All these data allow us
to construct theoretical models to account for its structure, looking for its
initial configuration and predicting its final fate. Assuming that the BH is
already formed when the primary star reaches the Zero Age Main Sequence, we
used our binary evolution code for such a purpose. We obtained that the present
characteristics of the system are nicely accounted for by a model with initial
masses of 9 solar masses for the BH, 1.5 solar masses for the companion star,
an initial orbital period of 1.5 d and considering that at most 30% of the mass
transferred by the donor is accreted by the BH. The metallicity of the donor
for our best fit was Z = 0.028 (twice solar metallicity). We also studied the
evolution of the BH spin parameter assuming that initially, it is not rotating.
Remarkably, the spin of the BHs in our models is far from reaching the
available observational determination. This may indicate that the BH in V404
Cyg is initially spinning, a result that may be relevant for understanding the
formation BHs in the context of LMXB systems.
