Ultraviolet light curves of beta Lyrae: Comparison of OAO A-2, IUE, and Voyager Observations

Kondo, Y.; McCluskey, G. E.; Silvis, Jeffery M. S.; Polidan, R. S.; Mccluskey, Carolina P. S.; Eaton, J. A.

doi:10.1086/173691

Cited by 22 publications

(30 citation statements)

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“…This is quite surprising, since the system is intrinsically non-axisymmetric. It is worth recalling that the UV lightcurve below Lyα is notable for lacking any eclipses as well (Kondo et al 1994). A somewhat analogous source to β Lyr is the near edge-on interacting binary W Ser.…”

Section: Discussionmentioning

confidence: 98%

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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 Motivated by an unpublished X-ray spectrum from the Einstein X-ray telescope suggesting unusually hard emission, we obtained time with Suzaku for pointings at three different phases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: 98%

“…1); however, the secondary minimum is deeper than the primary minimum at shorter wavelengths, and below Lyα the eclipses no longer appear (Kondo et al 1994). A summary of the system properties is given in Table 1.…”

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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“…In a recent paper, Linnell, Hubeny & Harmanec (1998b, hereafter Paper I) established a number of constraints on a possible model for β Lyrae. Paper I showed that the HP model is inconsistent with the UBV data of HMB and the OAO2 data of Kondo et al (1994). The small visible segment of the gainer leads to a stellar eclipse in the middle of secondary minimum, an eclipse that does not appear in the observations.…”

Section: Introductionmentioning

confidence: 96%

“…OAO2 photometry (Kondo et al 1994) has provided light curves in the near‐ and far‐UV. In combination with ground‐based photometry, the difference in depths of the minima, in progressing from a V light curve toward shorter wavelengths, becomes smaller until, at 1430 Å, the eclipse at 0.50 p (Min II) is marginally deeper than the eclipse at 0.0 p (Min I).…”

Section: Introductionmentioning

confidence: 99%

Progress on a model for β Lyrae

Linnell

2002

Monthly Notices of the Royal Astronomical Society

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It is generally accepted that β Lyrae is a massive mass‐transfer system in which the more massive gainer is embedded in a thick accretion disc. No detailed, quantitative accretion disc model of the system, which fits both the available photometric and spectroscopic data, has been published. This paper considers a thick accretion disc model. An empirical two‐temperature model for the accretion disc rim produces an accurate fit to the UBV and OAO2 photometry. The two‐temperature rim model leads to synthetic spectra with a much larger Balmer jump than is present in spectrophotometric scans. The same model fails to produce IR light curves with the 0.5p eclipse deeper than the 0.0p eclipse, as shown in the observations of Jameson & Longmore. The paper next reports initial results for a model in which an extra source of continuum radiation arises from Thomson scattering of radiation from the gainer, which is hidden from the observer by the thick accretion disc. The adopted rate of mass transfer cannot supply the energy radiated by the accretion disc rim, nor can any credible larger rate. The most likely energy source is the mass gainer.

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“…Cherepashchuk et al, 1984;Kondo et al, 1994). The Hipparcos astrometry mission obtained photometry at several hundred epochs for many bright stars, discovering 343 new eclipsing binary systems (Perryman et al, 1997).…”

Section: Eclipsing Binary Stars From Spacementioning

confidence: 99%

Space-Based Photometry of Eclipsing Binaries

Southworth¹

2011

Proc. IAU

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Abstract. I briefly review the history and prospects for the study of eclipsing binary star systems from space-based observatories. The benefits of shifting to space satellites lie in the high precision and cadence achievable, as well as the ability to access wavelength regions which are unattainable from the ground. Whilst small amounts of data on eclipsing binaries were obtained by the Voyager, IUE, OAO-II, Hipparcos and MOST, the more recent CoRoT and Kepler missions were the first to provide extensive data on large numbers of systems. The future holds the prospect of the PLATO satellite, which will go bigger, better and brighter.

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Ultraviolet light curves of beta Lyrae: Comparison of OAO A-2, IUE, and Voyager Observations

Cited by 22 publications

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

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

Progress on a model for β Lyrae

Space-Based Photometry of Eclipsing Binaries

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