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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 cannotaccrete at high rate, limited by the Eddington accretion rate, leading to theformation of an accretion disc. The theoretical model begins at the zero agemain sequence considering the rotation for both stars. For this purpose we usedthe stellar evolution code MESA, developed to calculate the evolution of starsin a wide range of parameters. We started the model adjusting fundamentalparameters published for this system through a chi-square optimizationalgorithm, and adopting an initial orbital period of 3.9 days and initialmasses for the primary component $M_{i,d} = 3.40$ $M_{\odot}$ and $M_{i,g}=3.18$ $M_{\odot}$ for the gainer, with a metallicity associated to this type ofDPV of $Z = 0.02$. The method converged successfully for eight free degrees and5% of confidence with a chi-square of $\Delta \chi^{2}_{0.95,8}= 0.212$. Wedescribe each evolutionary stage of both components until that the donorreaches 20% core helium depletion as stop criterion. We offer a complementaryanalysis for understanding the mechanism of the magnetic dynamos inside thedonor star using the Tayler-Spruit formalism. Currently, the theoretical modelis consistent with the fundamental parameters published for V495 Cen and wediscuss how our predictions can help to develop efficients theoretical modelsfor DPV stars.

Evolutionary process of the interacting binary V495 Centauri