A study of the interacting binary system V455 Cygni

Djurašević, G.; Vince, I.; Antokhin, I. I.; Shatsky, N. I.; Cséki, A.; Zakirov, M. M.; Eshankulova, M.

doi:10.1111/j.1365-2966.2011.20208.x

Cited by 2 publications

(2 citation statements)

References 20 publications

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“…Including these active regions in the model, we found significant improvements in the quality of the fit to observations. For further information about these active regions in the model, see Djurašević et al (2012).…”

Section: Radial Velocity Measurements and Spectroscopic Mass-ratiomentioning

confidence: 99%

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

Garrido

Mennickent

Djurašević

et al. 2012

Monthly Notices of the Royal Astronomical Society

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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.

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Section: Radial Velocity Measurements and Spectroscopic Mass-ratiomentioning

confidence: 99%

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

Garrido

Mennickent

Djurašević

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…The code has been successfully applied to several close binaries including the well-studied binary system β Lyrae (e.g. Djurašević et al 2010;Djurašević et al 2012;Garrido et al 2013;Mennickent et al 2012;). We assume that the disk is optically and geometrically thick and that its outer edge is approximated by a cylindrical surface.…”

Section: Model For An Optically Thick Disk Around the Gainermentioning

confidence: 99%

On the long-cycle variability of the Algol OGLE-LMC-DPV-065 and its stellar, orbital, and disc parameters

Mennickent

Cabezas

Djurašević

et al. 2019

Monthly Notices of the Royal Astronomical Society

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OGLE-LMC-DPV-065 is an interacting binary whose double-hump long photometric cycle remains hitherto unexplained. We analyze photometric time series available in archive datasets spanning 124 years and present the analysis of new high-resolution spectra. A refined orbital period is found of 10. d 0316267 ± 0. d 0000056 without any evidence of variability. In spite of this constancy, small but significant changes in timings of the secondary eclipse are detected. We show that the long period continuously decreases from 350 to 218 days during 13 years, then remains almost constant for about 10 years. Our study of radial velocities indicates a circular orbit for the binary and yields a mass ratio of 0.203 ± 0.001. From the analysis of the orbital light curve we find that the system contains 13.8 and 2.81 M stars of radii 8.8 and 12.6 R and absolute bolometric magnitudes -6.4 and -3.0, respectively. The orbit semimajor axis is 49.9 R and the stellar temperatures are 25460 K and 9825 K. We find evidence for an optically and geometrically thick disk around the hotter star. According to our model, the disk has a radius of 25 R , central and outer vertical thickness of 1.6 R and 3.5 R , and temperature of 9380 K at its outer edge. Two shock regions located at roughly opposite parts of the outer disk rim can explain the light curves asymmetries. The system is a member of the double periodic variables and its relatively high-mass and long photometric cycle make it similar in some aspects to β Lyrae.

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A study of the interacting binary system V455 Cygni

Cited by 2 publications

References 20 publications

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

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

On the long-cycle variability of the Algol OGLE-LMC-DPV-065 and its stellar, orbital, and disc parameters

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