Evolutionary process of the interacting binary V495 Centauri

We present a simple model for the double periodic variable (DPV) V495 Cen, which evolves as a binary system of intermediate mass, where the gainer cannot accrete at a high rate, limited by the Eddington accretion rate, leading to the formation of an accretion disc. The theoretical model begins at the zero-age main sequence considering the rotation for both stars. For this purpose we used the stellar evolution code MESA, developed to calculate the evolution of stars in a wide range of parameters. We started the model adjusting fundamental parameters published for this system through a chi-square optimization algorithm and adopting an initial orbital period of 3.9 d and initial masses M_i,d = 3.40 M_⊙ for the primary component and M_i,g = 3.18 M_⊙ for the gainer, with a metallicity associated with this type of DPV of Z = 0.02. The method converged successfully for 8 free degrees and 5 per cent of confidence with a chi-square of Δ χ ²_{0.95,8} = 0.212. We describe each evolutionary stage of both components until the donor reaches 20 per cent core helium depletion as the stop criterion. We offer a complementary analysis for understanding the mechanism of the magnetic dynamos inside the donor star using the Tayler-Spruit formalism. Currently, the theoretical model is consistent with the fundamental parameters published for V495 Cen and we discuss how our predictions can help to develop efficient theoretical models for DPV stars.