Physical parameters and evolutionary route for the Large Magellanic Cloud interacting binary OGLE 05155332−6925581★

Abstract

We analyze multicolor light curves and high resolution optical spectroscopy of the eclipsing binary and Double Periodic Variable OGLE 05155332-6925581. According to Mennickent et al., this system shows a significant change in the long non-orbital photometric cycle, a loop in the color-magnitude diagram during this cycle and discrete spectral absorption components that were interpreted as evidence of systemic mass loss. We find that the best fit to the multiband light curves requires a circumprimary optically thick disc with a radius about twice the radius of the more massive star. The spectroscopy indicates a mass ratio of 0.21 ± 0.02 and masses for the hot and cool stars of 9.1 ± 0.5 and 1.9 ± 0.2 M , respectively. A comparison with synthetic binary-star evolutionary models indicates that the system has an age of 4.76 × 10 7 years, is in the phase of rapid mass transfer, the second one in the life of this binary, in a Case-B mass-exchange stage. Donor-subtracted Hα profiles show the presence of double emission formed probably in an optically thin circumstellar medium, while the variable He I profile and the Hβ absorption wings are probably formed in the optically thick circumprimary disc. The model that best fit the observations shows the system with a relatively large mass transfer rate ofṀ = 3.1 × 10 −6 M /yr. However, the orbital period remains relatively stable during almost 15 years. This observation suggests that the hot-spot mass-loss model proposed by other authors is not adequate in this case, and that some other mechanism is efficiently removing angular momentum from the binary. Furthermore, our observations suggest that the DPV phenomenon could have an important effect in the balance of mass and angular momentum in the system.

Fundamental parameters of the close interacting binary HD 170582 and its luminous accretion disc

“…We find that HD 170882 shows spectroscopic properties similar to other DPVs like AU Monocerotis, V 393 Scorpii, DQ Velorum and OGLE 05155332-6925581 (Mennickent et al, 2008, 2012a, 2012b, Barría et al 2013, Garrido et al 2013. These properties include the existence of an optically thick disc surrounding a B-type star and evidence for stream-disc interaction.…”

“…More than 200 DPVs have been found in the Galaxy and the Magellanic Clouds (Mennickent 2013), but very few of them have been studied spectroscopically (e.g. Barría et al 2013, Garrido et al 2013. The study of HD 170852 is important to characterize DPVs in terms of their fundamental physical parameters and also to help to understand the still unknown cause for the long photometric cycle.…”

Orbital and superorbital periods in ULX pulsars, disc-fed HMXBs, Be/X-ray binaries, and double-periodic variables

“…Many papers discuss the spectroscopic observations of DPVs (e.g. Mennickent et al 2012;Barría et al 2014;Garrido et al 2013), all consisting of ∼2 M late B/early A-type mass donors (of radius ∼9 R ) rapidly transferring material onto ∼7-9 M early B-type primaries with circumstellar discs. This is remarkably close to what one would expect for progenitors of normal BeXRBs or Be + white dwarf systems.…”

Spectroscopic and photometric study of the eclipsing interacting binary V495 Centauri

“…Hitherto only a couple of DPVs, less than 5%, have been studied spectroscopically (e.g Mennickent et al (2008); a,b; Barría et al (2013Barría et al ( , 2014; Garrido et al (2013); Mennickent et al ( , 2016). 1 was discovered as a DPV by Mennickent & Rosales (2014), who find that the system is characterized by a long photometric cycle of 1283 d, resulting in the system with the longest period among Galactic DPVs.…”

“…Also, DPVs are considered as one specific evolutionary step for more massive Algols, one possibly involving mild mass transfer and systemic mass loss (Mennickent et al (2008)). An interesting property of these objects is the surprising constancy of their orbital periods, which is not expected in Algols undergoing RLOF mass transfer (Garrido et al (2013)). Also the DPVs seem to be hotter and more massive than classical Algols and seem to have always a B-type component; their orbital periods typically run between 4 and 100 days.…”