Progress on a model for β Lyrae

Linnell, Albert P.

doi:10.1046/j.1365-8711.2000.03898.x

Cited by 34 publications

(47 citation statements)

References 35 publications

(59 reference statements)

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“…A theoretical justification for the presence of bipolar jets was suggested by Bisikalo et al (2000). So far, the most successful modelling of the observed light curves, continuum distribution, and line spectra was carried out by Linnell (2000Linnell ( , 2002a. These studies also supported the view that there had to be scattering material above the disc.…”

Section: Introductionmentioning

confidence: 89%

“…BINSYN is one of the very few programs able to model the light curves of binaries with optically thick accretion discs 5 . Input parameters required by BINSYN were adopted from the study of Linnell (2000), who obtained the best fit of the observed light curves of β Lyr over a wide range of wavelengths so far. For details of the modelling we refer readers to Linnell (2000).…”

Section: Phase-locked Variations Of the Strength Of The Absorption Linesmentioning

confidence: 99%

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New findings supporting the presence of a thick disc and bipolar jets in the $\mathsf{\beta}$ Lyrae system

Chadima

Harmanec

et al. 2006

A&A

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Context. Understanding large-scale mass exchange in binaries also requires studies of complicated objects in the rapid phases of the process. β Lyr is one such object. Aims. Our goals were to analyse 52 photographic and 651 electronic spectra of β Lyr to obtain additional information about circumstellar matter and to investigate spectrophotometric information for the first time. Methods. Improved quadratic ephemeris was derived via orbital solution with the FOTEL program. The spectra were disentangled using the KOREL program. Spectrophotometric quantities of 15 stronger absorption lines of the primary were measured and corrected for the orbital continuum variations using the fluxes calculated from a fit of the light curves with the BINSYN program. Central intensities of the V and R peaks of the Hα emission line were measured and corrected for the orbital light changes using the R-band light curve numerically modelled with the program PERIOD04. Results. Disentangling of photographic and electronic spectra led to the detection of weak absorption lines originating from the pseudophotosphere of the accretion disc. This way, a rich line spectrum of the accretion disc, not limited to only two previously known Si ii 6347 and Si ii 6371 lines, was obtained. A projected rotational velocity of 180 km s −1 was estimated for the disc spectrum. Such a value agrees well with the assumption of the Keplerian rotation of the outer layers of the accretion disc. After the correction, a pronounced increase of the strength of all absorption lines around phases of the primary eclipse was found. We argue that this is due to additional absorption of the light of the primary in one of the jets and/or scattering envelope above the accretion disc of the gainer. The net intensity of the V peak of Hα shows no orbital variation, but a possible 271-d periodicity. The net intensity of the R peak shows mild orbital changes and a slow change over a cycle of about 2780 days. These results seem to support the earlier conclusion that the Hα emission originates in the jet-like structures. Conclusions. All new findings support the current picture that the circumstellar structures of β Lyr consist of a thick accretion disc, bipolar jets, and a scattering envelope above the disc.

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Section: Introductionmentioning

confidence: 89%

Section: Phase-locked Variations Of the Strength Of The Absorption Linesmentioning

confidence: 99%

New findings supporting the presence of a thick disc and bipolar jets in the $\mathsf{\beta}$ Lyrae system

Chadima

Harmanec

et al. 2006

A&A

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“…This required us to model an optically and geometrically thick disk surrounding the primary star. We used the BINSYN suite of programs (Linnell 1984;Linnell & Hubeny 1996;Linnell 2000) with a parameter optimization procedure based on the steepest descent method developed by DS. The optimization procedure controlled the flow of BINSYN software, automating the process.…”

Section: Light Curve Modelingmentioning

confidence: 99%

UX Monocerotis as a W Serpentis binary

Sudar

Harmanec

Lehmann

et al. 2011

A&A

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Using our new photometric and spectroscopic observations as well as all available published data, we present a new interpretation of the properties of the peculiar emission-line binary UX Mon. We conclude that this binary is in a rare phase of fast mass transfer between the binary components prior to the mass ratio reversal. We firmly establish that the orbital period is secularly decreasing at a rate ofṖ = −0.260 s per year. From several lines of reasoning, we show that the mass ratio of the component losing mass to the mass-gaining component q must be larger than 1 and find our most probable value to be q = 1.15 ± 0.1. The BINSYN suite of programs and the steepest descent method were used to perform the final modeling. We modeled the star as a W Ser star with a thick disk around its primary. Although the remaining uncertainties in some of the basic physical elements describing the system in our model are not negligible, the model is in fair agreement with available observations. Only the nature of the light variations outside the primary eclipse remains unexplained.

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“…Even if they provide a good model for the light curves in the near and far-UV and in the visible, they still do not predict the shape of the infrared light curve, and, in particular, they do not reproduce the secondary minimum that becomes deeper than the primary minimum at λ ≥ 4.8 µm. This leads to the conclusion that another component, besides stars plus accretion disk, must contribute to the observed flux, and Linnell (2000) proposes that the extra source of continuum radiation may be Thomson scattering of radiation from the gainer.…”

Section: Discussionmentioning

confidence: 99%

“…On the contrary very little is still known about the nature of the secondary nother than the fact that it should be embedded in an accretion disk. However, despite of the numerous efforts (Wilson 1974;Linnell & Hubeny 1996;Linnell et al 1998;Linnell 2000), there is no standard model of an accretion disk able to reproduce synthetic light curves that fit the observed ones from IR to UV. Therefore, we can compute the expected far-IR flux only for the primary component by assuming, between 1.5 × 10 16 and 1.5 × 10 12 Hz a Kurucz (1993) model with T eff = 13 000 K, log(g) = 3, as appropriate for the B8-6 II component.…”

Section: Stellar Wind/smentioning

confidence: 99%

The origin of the radio emission from β Lyrae

Umana

Leone

Trigilio

2002

A&A

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Abstract. In this paper we present new observational evidence that supports the presence of an extra source of continuum emission in the binary system β Lyrae. New VLA and IRAM observations, together with published data from the literature and ISO archive data, allow us to build the Spectral Energy Distribution of the binary between 5 × 10 9 Hz and 5 × 10 15 Hz. The radio-millimeter part of the spectrum is consistent with free-free emission from a symbiotic-like wind associated with the primary component and ionized by the radiation field of the hidden companion. Furthermore, we also consider the possibility that the observed radio flux originates from collimated radio structures associated with the mass gaining component and its disk (Conical thermal jets). An extrapolation of this emission to the far-IR part of the spectrum indicates that in both cases the free-free contribution at these frequencies cannot explain the observations and that the observed infrared excess flux is due principally to the secondary component and its associated disk.

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Progress on a model for β Lyrae

Cited by 34 publications

References 35 publications

New findings supporting the presence of a thick disc and bipolar jets in the $\mathsf{\beta}$ Lyrae system

New findings supporting the presence of a thick disc and bipolar jets in the $\mathsf{\beta}$ Lyrae system

UX Monocerotis as a W Serpentis binary

The origin of the radio emission from β Lyrae

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