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To progress in the comprehension of the double periodic variable (DPV)phenomenon, we analyse a series of optical spectra of the DPV system DQ Velorumduring much of its long-term cycle. In addition, we investigate theevolutionary history of DQ Vel using theoretical evolutionary models to obtainthe best representation for the current observed stellar and orbital parametersof the binary. We investigate the evolution of DQ Vel through theoreticalevolutionary models to estimate the age and the mass transfer rate which arecompared with those of its twin V393 Scorpii. Donor subtracted spectra coveringaround 60% of the long-term cycle, allow us to investigate time-modulatedspectral variations of the gainer star plus the disc. We compare the observedstellar parameters of the system with a grid of theoretical evolutionary trackscomputed under a conservative and a non-conservative evolution regime. We havefound that the EW of Balmer and helium lines in the donor subtracted spectraare modulated with the long-term cycle. We observe a strenghtening in the EWsin all analysed spectral features at the minimum of the long-term cycle whichmight be related to an extra line emission during the maximum of the long-termvariability. Difference spectra obtained at the secondary eclipse support thisscenario. We have found that a non-conservative evolutionary model is a betterrepresentation for the current observed properties of the system. The bestevolutionary model suggests that DQ Vel has an age of 7.40 x 10^{7} yr and iscurrently in a low mass transfer rate (-9.8x10^{-9} Msun/yr) stage, after amass transfer burst episode. Comparing the evolutionary stages of DQ Vel andV393 Sco we observed that the former is an older system with a lower masstransfer rate. This might explain the differences observed in the physicalparameters of their accretion discs.

Exploring the long-term variability and evolutionary stage of the interacting binary DQ Velorum