The ultraviolet spectrum of Beta Lyrae. II

Hack, Margherita; Tulloch, M. K.; Hutchings, J. B.; Kondo, Y.; McCluskey, G. E.

doi:10.1086/154438

Cited by 17 publications

(9 citation statements)

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“…Table 4 gives the radial velocity of the absorption cores of the enve lope lines for Beta Lyr. Their behavior is strictly similar to that observed with Copernicus in 1973 and 1974 by Hack et al (1975Hack et al ( , 1976 for the lines included in the spectral range 1030-1400 A. 278 M. HACK ET AL.…”

Section: Radial Velocitiessupporting

confidence: 81%

IUE Observations of the Two Peculiar Binary Systems Beta Lyrae and Upsilon Sagittarii

Hack

Flora

Santin

1980

Symp. - Int. Astron. Union

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The common peculiarities of these two systems are: a) the companion is a massive object (probably m2≥10) whose spectrum is not observable; b) both systems show evidence, though in different degrees, of mass-transfer and mass-loss; c) both present, in different degrees, hydrogen deficiency; d) ultraviolet observations have shown, in both cases, the presence of lines of highly ionized elements like N V, C IV, Si IV, probably formed in an extended envelope because they do not show orbital radial velocity shifts, and cannot be explained by the effective temperature of the star whose spectrum we observe. The latter property seems to be common to several close binaries, as shown by the ultraviolet observations with IUE by Plavec and Koch (1979); e) both systems present infrared excess, suggesting the presence of an extended envelope (Gehrz et al. 1974; Lee and Nariai, 1967; Humphreys and Ney, 1974; Treffers et al. 1976).

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Section: Radial Velocitiessupporting

confidence: 81%

IUE Observations of the Two Peculiar Binary Systems Beta Lyrae and Upsilon Sagittarii

Hack

Flora

Santin

1980

Symp. - Int. Astron. Union

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“…Many authors have discussed the possibility of a coronal structure associated with β Lyrae (Kriz 1974; Jameson & Longmore 1976; Hack et al 1976a,b, 1977; Viotti et al 1978). Wilson & Lapasset (1981) discuss the possible effects of a corona overlying the accretion disc proper, and call for quantitative results in connection with proposed β Lyrae models.…”

Section: A Light‐scattering Modelmentioning

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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“…According to Hack et al (1975Hack et al ( , 1976Hack et al ( , 1977 β-Lyr is a complex system consisting of a B 8 primary star, an unknown companion, an envelope and a disk. The FUV spectrum is dominated by high ionization emission lines…”

Section: Fuv Variabilitymentioning

confidence: 99%

UVSTAR observations of Adara (ϵ CMa): 575–1250 Å

Gregorio

Stalio

Broadfoot

et al. 2002

A&A

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Abstract. UVSTAR, UltraViolet Spectrograph Telescope for Astronomical Research, operates in the 500-1250Å wave-band at 1 to 3Å resolution. Here we report on the EUV and FUV observations of the B2 II star Adara, the brightest EUV source in the sky, obtained by UVSTAR during the STS 69 and STS 95 missions. The discussion concerns 1) wavelength and flux calibration, 2) short term time variability of selected spectral features, 3) comparison with previous measurements in the EUV band and 4) comparison with model atmospheres.

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The ultraviolet spectrum of Beta Lyrae. II

Cited by 17 publications

References 0 publications

IUE Observations of the Two Peculiar Binary Systems Beta Lyrae and Upsilon Sagittarii

IUE Observations of the Two Peculiar Binary Systems Beta Lyrae and Upsilon Sagittarii

Progress on a model for β Lyrae

UVSTAR observations of Adara (ϵ CMa): 575–1250 Å

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