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We analyze multicolor light curves and high resolution optical spectroscopyof the eclipsing binary and Double Periodic Variable OGLE 05155332-6925581.According to Mennickent et al., this system shows a significant change in thelong non-orbital photometric cycle, a loop in the color-magnitude diagramduring this cycle and discrete spectral absorption components that wereinterpreted as evidence of systemic mass loss. We find that the best fit to themulti-band light curves requires a circumprimary optically thick disc with aradius about twice the radius of the more massive star. The spectroscopyindicates a mass ratio of 0.21+-0.02 and masses for the hot and cool stars of9.1+-0.5 and 1.9+-0.2 M_sun, respectively. A comparison with syntheticbinary-star evolutionary models indicates that the system has an age of 4.76E7years, is in the phase of rapid mass transfer, the second one in the life ofthis binary, in a Case-B mass-exchange stage. Donor-subtracted H_alpha profilesshow the presence of double emission formed probably in an optically thincircumstellar medium, while the variable HeI profile and the H_beta absorptionwings are probably formed in the optically thick circumprimary disc. The modelthat best fit the observations shows the system with a relatively large masstransfer rate of dM/dt = 3.1E-6 M_sun/yr. However, the orbital period remainsrelatively stable during almost 15 years. This observation suggests that thehot-spot mass-loss model proposed by other authors is not adequate in thiscase, and that some other mechanism is efficiently removing angular momentumfrom the binary. Furthermore, our observations suggest that the DPV phenomenoncould have an important effect in the balance of mass and angular momentum inthe system.

Physical parameters and evolutionary route for the LMC interacting binary OGLE 05155332-6925581