Three-dimensional hydrodynamical modeling of mass transfer in the close binary system β Lyr

Nazarenko, Sergey; Glazunova, L. V.

doi:10.1134/s1063772906050040

Cited by 17 publications

(18 citation statements)

References 5 publications

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“…It is unclear whether this model can generate gas at temperatures high enough to produce the observed X-rays. Hydrodynamic modeling of the β Lyr system has also been pursued by Nazarenko & Glazunova (2003, 2006a, first in 2D simulations and then in 3D simulations. These researchers included cooling curves in their simulations and allowed for a stellar wind by the gainer.…”

Section: Discussionmentioning

confidence: 99%

“…Despite numerous and ongoing modeling attempts (e.g., Wilson 1974;Linnell & Hubeny 1996;Bisikalo et al 2000;Linnell 2002;Nazarenko & Glazunova 2003, 2006a, no model is capable yet of matching the observed light curves of β Lyr from the IR through the UV. Strangely, β Lyr has largely been left unstudied in the X-ray regime, despite the strong X-ray flux detected by the ROSAT HRI (Berghöfer & Schmitt 1994).…”

Section: Introductionmentioning

confidence: 99%

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Phase-dependent X-ray observations of the β Lyrae system

Ignace

Oskinova

Waldron

et al. 2007

A&A

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Aims. We report on observations of the eclipsing and interacting binary β Lyrae from the Suzaku X-ray telescope. This system involves an early B star embedded in an optically and geometrically thick disk that is siphoning atmospheric gases from a less massive late B II companion. Methods. Motivated by an unpublished X-ray spectrum from the Einstein X-ray telescope suggesting unusually hard emission, we obtained time with Suzaku for pointings at three different phases within a single orbit. Results. From the XIS detectors, the softer X-ray emission appears typical of an early-type star. What is surprising is the remarkably unchanging character of this emission, both in luminosity and in spectral shape, despite the highly asymmetric geometry of the system. We see no eclipse effect below 10 keV. The constancy of the soft emission is plausibly related to the wind of the embedded B star and Thomson scattering of X-rays in the system, although it might be due to extended shock structures arising near the accretion disk as a result of the unusually high mass-transfer rate. There is some evidence from the PIN instrument for hard emission in the 10-60 keV range. Follow-up observations with the RXTE satellite will confirm this preliminary detection.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Phase-dependent X-ray observations of the β Lyrae system

Ignace

Oskinova

Waldron

et al. 2007

A&A

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“…All of these properties suggest that HDE 326823 is an interacting binary which is experiencing active mass transfer. Here we propose that HDE 326823 is related to the W Serpentis class of massive binaries (Tarasov 2000), systems in which the mass donor appears as the visible, lower mass component and the more massive mass gainer is hidden behind a thick accretion torus (Nazarenko & Glazunova 2006). The mass function f (M) (Table 2) indicates that the total mass of the system is large,…”

Section: Discussionmentioning

confidence: 99%

A Binary Orbit for the Massive, Evolved Star Hde 326823, a Wr+o System Progenitor

Richardson

Gies

2011

The Astronomical Journal

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The hot star HDE 326823 is a candidate transition-phase object that is evolving into a nitrogen-enriched Wolf-Rayet star. It is also a known low-amplitude, photometric variable with a 6.123 day period. We present new, high-and moderate-resolution spectroscopy of HDE 326823, and we show that the absorption lines show coherent Doppler shifts with this period while the emission lines display little or no velocity variation. We interpret the absorption line shifts as the orbital motion of the apparently brighter star in a close, interacting binary. We argue that this star is losing mass to a mass gainer star hidden in a thick accretion torus and to a circumbinary disk that is the source of the emission lines. HDE 326823 probably belongs to a class of objects that produce short-period WR+O binaries.

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“…This active region could be interpreted as the effect of a disk-shaped deviation from the circular one, i.e., as a hump on the disk edge from which part of the disk material probably leaves the system. An additional interpretation of the bright-spot nature can be found in recent gasodynamical studies, e.g., Heemskerk (1994), Bisikalo et al (1998Bisikalo et al ( , 2000, Harmanec et al (2002), Nazarenko & Glazunova (2003, 2006a, 2006b, showing very complicated gas flows in the system and the complex structure of the disk. It is reasonable to expect that part of the gas stream and the disk material from this active region leave the system into the surrounding space, possibly forming a kind of circumbinary envelope.…”

Section: Observations and Modelmentioning

confidence: 99%

“…The conical form of the disk surface is described by the disk radius (R d ), and by the disk thicknesses at the edge (d e ) and at the center of the disk (d c ). This is a rough approximation of the disk shape obtained by the current hydrodynamical modeling of mass transfer in close binary systems; see, e.g., Bisikalo et al (2000), Harmanec et al (2002), and Nazarenko & Glazunova (2003, 2006a, 2006b.…”

Section: Observations and Modelmentioning

confidence: 99%

Accretion Disk in the Massive Binary Ry Scuti

Djurašević

Vince

Atanackovic

2008

The Astronomical Journal

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The UBVR light curves of the massive eclipsing binary RY Sct, obtained at the Maidanak Observatory from 1979 to 1992, have been re-analyzed in order to prove the hypothesis of the presence of an accretion disk in the system. This hypothesis is supported by a new spectroscopic study of Grundstrom et al., and by a specific light-curve shape exhibiting a slight asymmetry around the secondary minima and a small difference in the height of the successive maxima. The light-curve analysis was performed using a Roche model of a binary containing a geometrically and optically thick accretion disk around the more massive primary star. By solving the inverse problem, the orbital elements and the physical parameters of the system components and of the accretion disk were estimated for all the individual UBVR light curves. The model gives a consistent solution for the RY Sct binary system and supports the hypothesis of the existence of an optically thick disk around the massive component. Our results suggest a mass exchange between the components and a mass loss from the system. This could be considered as a possible mechanism of the formation of the accretion disk around the more massive component and of the circumbinary envelope of toroidal form in the orbital plane of the system.

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Three-dimensional hydrodynamical modeling of mass transfer in the close binary system β Lyr

Cited by 17 publications

References 5 publications

Phase-dependent X-ray observations of the β Lyrae system

Phase-dependent X-ray observations of the β Lyrae system

A Binary Orbit for the Massive, Evolved Star Hde 326823, a Wr+o System Progenitor

Accretion Disk in the Massive Binary Ry Scuti

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