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

Abstract

AG Draconis produces a strong supersoft X-ray emission.The X-ray and optical/UV fluxes are in a strict anticorrelation throughout the active and quiescent phases. The aim of this contribution is to identify the source of the X-ray emission and reveal the nature of the observed flux anticorrelation. For this purpose we model the 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. Our analysis showed that 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.

9 pages, 2 figures, 3 tables. Submitted to AA on 25/11/2008, revised on 27/05/2009

References in corpus (5)

• Broad H-alpha wings from the optically thin stellar wind of the hot components in symbiotic binaries
• On the effect of emission lines on the UBVR photometry
• Structure of the hot object in the symbiotic prototype Z And during its 2000-03 active phase
• Recent photometry of symbiotic stars - XII
• The origin of the supersoft X-ray--optical/UV flux anticorrelation in the symbiotic binary AG Draconis

Cited by in corpus (18)

• An Online Catalog of Cataclysmic Variable Spectra from the Far Ultraviolet Spectroscopic Explorer
• The origin of the supersoft X-ray--optical/UV flux anticorrelation in the symbiotic binary AG Draconis
• New outburst of the symbiotic nova AG Peg after 165 years
• Multiwavelength modelling the SED of supersoft X-ray sources. I. The method and examples
• Formation of a disk structure in the symbiotic binary AX Per during its 2007-10 precursor-type activity
• Swift observations of the 2015 outburst of AG Peg -- from slow nova to classical symbiotic outburst
• Electron optical depths and temperatures of symbiotic nebulae from Thomson scattering
• Ionization structure of hot components in symbiotic binaries during active phases
• The path to Z And-type outbursts: The case of V426 Sagittae (HBHA 1704-05)
• OGLE-SMC-LPV-00861 (LIN 9): the first proven Z And outburst in a Magellanic symbiotic star
• An X-Ray and Optical Light Curv Model of the Eclipsing Symbiotic Binary SMC3
• Detection of X-rays from the jet-driving symbiotic star Hen 3-1341
• Outburst activity of symbiotic system AGDra
• Broad Observational Perspectives Achieved by the Accreting White Dwarf Sciences in the XMM-Newton and Chandra Eras
• Multiwavelength modeling the SED of Luminous Supersoft X-ray Sources in Large Magellanic Cloud and Small Magellanic Cloud
• The symbiotic system AG Draconis. Soft X-ray bremsstrahlung from the nebulae
• Photometry of Symbiotic Stars - XIV
• The long-term spectroscopic misadventures of AG Dra with a nod toward V407 Cyg: Degenerates behaving badly