Model for the long and orbital brightness variability of the <i>β</i> Lyrae type binary OGLE-BLG-ECL-157529

Mennickent, R. E.; Djurašević, G.

doi:10.1051/0004-6361/202141098

Cited by 3 publications

(1 citation statement)

References 38 publications

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“…We note that a hotter disk during maximum was predicted by a simpler study in the past (Djurašević 1993). Contrarily, (Mennickent & Djurašević 2021). On the other hand, the system OGLE-LMC-DPV-097 is characterized by a long-cycle length of ∼ 306 days and an amplitude of ∼ 0.8 mag in the I band.…”

Section: Discussionmentioning

confidence: 67%

Cyclic changes in the interacting binary RX Cassiopeiae

Mennickent

Djursevic

Petrović

et al. 2022

A&A

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We analyzed 109 years of published photometry and times of minima of the eclipsing interacting binary RX Cas. The inclusion of 171 previously unnoticed minima confirms the tendency of an increase in the orbital period at a rate of 1.84 seconds per cycle. We also find evidence of variations in the length of the previously reported long photometric cycle and changes in the shape of the orbital light curve. By modeling the orbital light curves at different epochs, and assuming symmetry in the system physical conditions during the first and second halves of the long cycle, we find that the changes in the orbital light curve can be explained by variations in the physical properties of the accretion disk. We find that epochs of maximum brightness are those of thicker and hotter disks. In addition, we explore the evolutionary history of the system using the Modules for Experiments in Stellar Astrophysics code and find that the binary can be the result of nonconservative evolution of two stars of very similar initial mass (around 5.5 M ) and orbital period of 4 days, although less massive and conservative models of longer starting orbital periods cannot be discarded.

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Section: Discussionmentioning

confidence: 67%

Cyclic changes in the interacting binary RX Cassiopeiae

Mennickent

Djursevic

Petrović

et al. 2022

A&A

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V4142 Sgr: Double periodic variable with an accretor surrounded by the accretion disk’s atmosphere

Rosales

Mennickent

Djurašević

et al. 2023

A&A

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Context. A detailed study of the close interacting binary V4142 Sgr, based on photometric and spectroscopic analyses, indicates that this system belongs to the enigmatic class of Algol-like variables exhibiting a long photometric cycle of an unknown nature. Aims. By performing photometric data-mining and spectroscopic observations covering the orbital cycle, we obtained the orbital parameters and the stellar properties of the binary system, along with the physical properties of the accretion disk located around the hot star. In addition, we gained insights into the evolutive path of the system. Methods. We modeled the light curve through an inverse method, using a theoretical light curve of the binary system that considers the light curve contribution of both stars and the accretion disk of the hot star to obtain the fundamental parameters. To constrain the main stellar parameters, the mass ratio was fixed in addition to the donor temperature, using the obtained values from our spectroscopic analysis, which includes deblending methods to isolate the spectral lines of the stellar components. The system parameters were compared with a grid of binary star evolutive models in order to gain insights into the evolutionary history of the system. Results. The orbital period and the long cycle were re-calculated, with the following result: 30 d .633 ± 0 d .002 and 1201 ± 14 days. The spectral analysis reveals Hα double emission with a persistent V ≤ R asymmetry, which is considered evidence of a possible wind emerging from the hotspot region. In addition, a cold and evolved donor star of M d = 1.11 ± 0.2 M , T d = 4500 ± 125 K and a R d = 19.4 ± 0.2 R as well as a rejuvenated B-dwarf companion of M g = 3.86 ± 0.3 M , T g = 14380 ± 700 K, and R g = 6.35 ± 0.2 R were found. The gainer is surrounded by a concave and geometrically thick disk, creating its own atmosphere around the main component of a radial extension, R d = 22.8 ± 0.3 R , contributing ∼ 1.4 percent of the total luminosity of the system at the V-band at orbital phase 0.25. The disk is characterized by a hot-spot roughly placed where the stream hits the disk and an additional bright-spot separated 102. • 5 ± 0. • 04 degrees along the disk edge rim in the direction of the orbital motion. The system is seen under an inclination of 81. • 5 ± 0. • 3 and at a distance of d Gaia = 1140 ± 35 pc. Doppler maps of the emission lines reveal sites of enhanced line emission in the second and third velocity quadrants. The former would correspond to a hotspot and the latter to a bright spot detected by the light curve analysis. We find that the system comes from an initially shorter orbital period binary that inverted its mass ratio due to mass exchange. A plausible model scenario indicates that, at present, the K-type giant should have been depleted of hydrogen in its core, while the companion would have gained about 2 M through a process lasting about 2 Myr.

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Accretion Disks and Long Cycles in β Lyrae-Type Binaries

Mennickent¹

2022

Galaxies

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In order to inquire about the nature of the accretion disks formed around the more massive companion in binaries with β Lyrae-type light curves, we review literature presenting some physical and observational properties of these systems. In addition, we inspect the photometric time series of three representative eclipsing systems obtained by the Optical Gravitational Lensing Experiment (OGLE) project during the last decades and compare them with β Lyrae. All these three systems show indications of being semidetached with a more massive B-type component and in a mass transfer stage. They also show long photometric cycles, and two of them show changes in the orbital light curve that can be interpreted in terms of structural changes of the accretion disks, eventually driven by variations in the mass transfer rate.

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Model for the long and orbital brightness variability of the β Lyrae type binary OGLE-BLG-ECL-157529

Cited by 3 publications

References 38 publications

Cyclic changes in the interacting binary RX Cassiopeiae

Cyclic changes in the interacting binary RX Cassiopeiae

V4142 Sgr: Double periodic variable with an accretor surrounded by the accretion disk’s atmosphere

Accretion Disks and Long Cycles in β Lyrae-Type Binaries

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