This work of thesis aims to study the properties of the recurrent nova RS Ophiuchi, whose latest outburst phase was observed in August 2021. RS Ophiuchi is a binary system composed of a red giant star and a CO white dwarf (WD). These stars are close enough to have the transfer of matter from the red giant to the WD. The accretion of this matter on the surface of the WD gives rise to recurrent releases of energy by a thermonuclear runaway. Simulations of the nova RS Ophiuchi were made with MESA (Modules for Experiments in Stellar Astrophysics) star module as a part of the NuGrid (Nucleosynthesis Grid) collaboration’s collection of software tools for simulations. Two different simulations were made for the WD profile with and without convective boundary mixing. For each WD profile, WD models for different evolutionary paths were made, resulting in WD models with different masses of the accreted shells. For the logarithmic luminosity of the RS Ophiuchi, a value of log10 L L⊙ = 1.867, has been obtained, and comparison with the logarithmic luminosity of models in plots of constant WD Roche lobe radius brought me to the conclusion that RS Ophiuchi has a greater mass of the accreted envelope than most models. Models with logarithmic luminosity close to the one of RS Ophiuchi of both profiles have both pp-chain, and CNO cycles ignited in their accreted envelope, confirming that these models are good models of the nova RS Ophiuchi.