Evolution of the symbiotic binary system AG Dranconis

Mikołajewska, Joanna; Kenyon, Scott J.; Mikołajewski, M.; Garcia, M. R.; Polidan, R. S.

doi:10.1086/117361

Cited by 58 publications

(94 citation statements)

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“…Indeed, LMC S63 was detected at the 5σ level by the ROSAT PSPC survey in September 7-December 17, 1990 (φ = 0.35 − 0.45; Bickert, Stencel & Luthardt 1993). The flux corrected for vignetting was 0.0112 counts/sec which is ∼140 times less than the flux of AG Dra observed at quiescence on Nov 27-Dec 7 (Bickert et al 1993), at orbital phase φ ∼ 0.7 and L h ∼ 1000 (d/2.5 kpc) 2 (Mikołajewska et al 1995). After scaling the AG Dra flux to the distance of the LMC (Pietrzyński et al 2013) its flux should be equal to ∼0.00385 counts/sec, ∼3 times fainter than LMC S63.…”

Section: The Hot Componentmentioning

confidence: 79%

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

Iłkiewicz

Mikołajewska

Miszalski

et al. 2015

Mon. Not. R. Astron. Soc.

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We present an analysis of multi-epoch low-resolution spectrophotometry, complemented by the light curves provided by massive photometric surveys spanning over 100 years, of the symbiotic binary LMC S63. We showed that it is an eclipsing binary with the orbital period of 1050 d . We also found evidence of outbursts in history of the white dwarf. If it was a Z-And type outburst, as is most likely, it would be a second such outburst recorded in the Magellanic Cloud symbiotic system. We confirmed that the red giant is enhanced in carbon, and estimated C/O ≃ 1.2 by fitting a model atmosphere to the SALT spectrum. We also found bi-periodic pulsations of the red giant, and demonstrated that it is similar to other carbon variables with confirmed bi-periodicity.

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Section: The Hot Componentmentioning

confidence: 79%

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

Iłkiewicz

Mikołajewska

Miszalski

et al. 2015

Mon. Not. R. Astron. Soc.

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“…These last mentioned authors suggest that the O vi P Cygni absorption is only that of the resonance doublet, superposed on a false continuum, produced by electron scattering wings. We may finally note that the geometry of this system with a fairly small preferred orbital inclintion of 30-45 • according to Mikołajewska et al (1995) as well as a low metal abundance, may play roles in reducing shifts between the resonance and intercombination lines.…”

Section: Clues About the Nature Of The Observed Radial Velocity Shiftmentioning

confidence: 83%

UV emission line shifts of symbiotic binaries

Friedjung¹,

Mikołajewska²,

Zajczyk³

et al. 2010

A&A

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Aims. Relative and absolute emission line shifts have been previously found for symbiotic binaries, but their cause was not clear. This work aims to better understand the emission line shifts. Methods. Positions of strong emission lines were measured on archival UV spectra of Z And, AG Dra, RW Hya, SY Mus and AX Per and relative shifts between the lines of different ions compared. Profiles of lines of RW Hya and Z And were also examined.Results. The reality of the relative shift between resonance and intercombination lines of several times ionised atoms was clearly shown except for AG Dra. This redshift shows a well defined variation with orbital phase for Z And and RW Hya. In addition the intercombination lines from more ionised atoms and especially O iv are redshifted with respect to those from less ionised atoms.Other effects are seen in the profiles. Conclusions. The resonance-intercombination line shift variation can be explained in quiescence by P Cygni shorter wavelength component absorption, due to the wind of the cool component, which is specially strong in inferior conjunction of this cool giant. The velocity stratification permits absorption of line emission. The relative intercombination line shifts may be connected with varying occultation of line emission near an accretion disk, which is optically thick in the continuum.

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“…González-Riestra et al 2008). Considering the geometry of the main sources of radiation, Mikolajewska et al (1995) estimated a system inclination i ≈ 30 • −45 • and Schmid & Schild (1997), based on spectropolarimetric observations, suggested i = 60 ± 8.…”

Section: Figmentioning

confidence: 99%

“…During the optical maxima, the soft X-ray emission was not detectable (long dashed lines). Mikolajewska et al (1995) re-analyzed several IUE spectra and suggested E B−V = 0.05 ± 0.01, while Birriel et al (2000) derived the extinction value of E B−V = 0.08 ± 0.01 mag by fitting the UV spectra obtained by the Hopkins Ultraviolet Telescope. These quantities are comparable to the total reddening through the Galaxy towards AG Dra (0.07-0.08, Burstein & Heiles 1982), which justifies that the measured extinction to AG Dra is purely interstellar.…”

Section: Figmentioning

confidence: 99%

The origin of the supersoft X-ray-optical/UV flux anticorrelation in the symbiotic binary AG Draconis

Skopal¹,

Sekeráš²,

González‐Riestra

et al. 2009

A&A

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Context. AG Draconis produces a strong supersoft X-ray emission. The X-ray and optical/UV fluxes are in strict anticorrelation throughout the active and quiescent phases. Aims. We identify the source of the X-ray emission and reveal the nature of the observed flux anticorrelation. Methods. We used X-ray and UV observations with XMM-Newton, far-UV spectroscopy from FUSE, low-and high-resolution IUE spectra, and optical/near-IR spectroscopic and/or photometric observations. We modeled the spectral energy distribution and broad wings of the O vi λ1032, λ1038 and He ii λ1640 lines by the electron-scattering during the maximum of the 2003 burst, and the subsequent transition and quiescent phase. Results. The X-ray-near-IR energy distribution at different levels of the star's brightness confirmed the observed flux anticorrelation quantitatively and showed that the optical bursts are associated to an increase in the nebular component of radiation. The profile-fitting analysis revealed a significant increase in the mean particle density around the hot star from ∼2.6 × 10 10 cm −3 during quiescent phase to ∼1.1 × 10 12 cm −3 during the burst. Conclusions. The supersoft X-ray emission is produced by the white dwarf photosphere. The X-ray and far-UV fluxes make it possible to determine its temperature unambiguously. The supersoft X-ray-optical/UV flux anticorrelation is caused by the variable wind from the hot star. The enhanced hot star wind gives rise to the optical bursts by reprocessing high-energy photons from the Lyman continuum to the optical/UV.

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Evolution of the symbiotic binary system AG Dranconis

Cited by 58 publications

References 0 publications

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

UV emission line shifts of symbiotic binaries

The origin of the supersoft X-ray-optical/UV flux anticorrelation in the symbiotic binary AG Draconis

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