DETECTION OF X-RAYS FROM THE SYMBIOTIC STAR V1329 Cyg

Stute, Matthias; Luna, G. J. M.; Sokoloski, J. L.

doi:10.1088/0004-637x/731/1/12

Cited by 10 publications

(10 citation statements)

References 26 publications

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“…The optical spectra discussed in §2.2 show evidence for extended wing features in the Balmer line emission during the 2015 outburst. For X-ray temperatures <1keV, we would expect shock speeds slower than 1000 km/s (see eqn 4 of Stute, Luna & Sokoloski 2011), consistent with the optical line widths. Taking a Bremsstrahlung cooling time of: tBremss = ( T 2 × 10 6 K) 1/2 ( n 3 × 10 9 cm −3 ) ∼ days (1) (Frank, King, & Raine 1992), the rapid X-ray variability suggests that the shocked gas was probably quite dense.…”

Section: The Origin Of the X-ray Emissionsupporting

confidence: 64%

Swiftobservations of the 2015 outburst of AG Peg – from slow nova to classical symbiotic outburst

Ramsay

Sokoloski

Luna

et al. 2016

Mon. Not. R. Astron. Soc.

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Symbiotic stars often contain white dwarfs with quasi-steady shell burning on their surfaces. However, in most symbiotics, the origin of this burning is unclear. In symbiotic slow novae, however, it is linked to a past thermonuclear runaway. In June 2015, the symbiotic slow nova AG Peg was seen in only its second optical outburst since 1850. This recent outburst was of much shorter duration and lower amplitude than the earlier eruption, and it contained multiple peaks -like outbursts in classical symbiotic stars such as Z And. We report Swift X-ray and UV observations of AG Peg made between June 2015 and January 2016. The X-ray flux was markedly variable on a time scale of days, particularly during four days near optical maximum, when the X-rays became bright and soft. This strong X-ray variability continued for another month, after which the X-rays hardened as the optical flux declined. The UV flux was high throughout the outburst, consistent with quasi-steady shell burning on the white dwarf. Given that accretion disks around white dwarfs with shell burning do not generally produce detectable X-rays (due to Compton-cooling of the boundary layer), the X-rays probably originated via shocks in the ejecta. As the X-ray photoelectric absorption did not vary significantly, the X-ray variability may directly link to the properties of the shocked material. AG Peg's transition from a slow symbiotic nova (which drove the 1850 outburst) to a classical symbiotic star suggests that shell burning in at least some symbiotic stars is residual burning from prior novae.

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Section: The Origin Of the X-ray Emissionsupporting

confidence: 64%

Swiftobservations of the 2015 outburst of AG Peg – from slow nova to classical symbiotic outburst

Ramsay

Sokoloski

Luna

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Repeating X-ray observations, as recently performed by Stute et al (2011), should help to locate the X-ray source in the binary.…”

Section: V1329 Cygmentioning

confidence: 93%

Recent photometry of symbiotic stars

et al. 2012

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We present new multicolour (UBVRCIC) photometric observations of classical symbiotic stars, EG And, Z And, BF Cyg, CH Cyg, CI Cyg, V1329 Cyg, TX CVn, AG Dra, Draco C1, AG Peg, and AX Per, carried out between 2007.1 and 2011.9. The aim of this paper is to present new data of our monitoring programme, to describe the main features of their light curves (LC) and to point problems for their future investigation. The data were obtained by the method of the classical photoelectric and CCD photometry.

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“…On the other hand, many classical symbiotic stars have also been detected as X-ray sources (e.g. Mürset, Wolff & Jordan , 1997;Wheatley, Mukai, & de Martino , 2003;Stute, Luna & Sokoloski , 2011), as a natural consequence of their hot component properties, (T h 10 5 K, L h ∼ 10 3 − 10 4 L ⊙ , e.g. Mürset et al , 1991;Skopal , 2005).…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength modelling the SED of supersoft X-ray sources I. The method and examples

Skopal

2015

New Astronomy

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-New method of modelling the spectra of supersoft X-ray sources is introduced. -The method analyses the X-ray/near-IR spectral energy distribution. -The multiwavelength approach overcomes problems of modelling only the X-ray data. -More trustworthy fundamental parameters are derived. AbstractRadiation of supersoft X-ray sources (SSS) dominates both the supersof X-ray and the far-UV domain. A fraction of their radiation can be reprocessed into the thermal nebular emission, seen in the spectrum from the near-UV to longer wavelengths. In the case of symbiotic X-ray binaries (SyXBs) a strong contribution from their cool giants is indicated in the optical/near-IR. In this paper I introduce a method of multiwavelength modelling the spectral energy distribution (SED) of SSSs from the supersoft X-rays to the near-IR with the aim to determine the physical parameters of their composite spectra. The method is demonstrated on two extragalactic SSSs, the SyXB RX J0059.1-7505 (LIN 358) in the Small Magellanic Cloud (SMC), RX J0439.8-6809 in the Large Magellanic Cloud (LMC) and two Galactic SSSs, the classical nova RX J2030.5+5237 (V1974 Cyg) during its supersoft phase and the classical symbiotic star RX J1601.6+6648 (AG Dra) during its quiescent phase. The multiwavelength approach overcomes the problem of the mutual dependence between the temperature, luminosity and amount of absorption, which appears when only the X-ray data are fitted. Thus, the method provides an unambiguous solution. It was found that selection of the model (a blackbody or an atmospheric model) is not of crucial importance in fitting the global X-ray/IR SED. The multiwavelength modelling of the SED of SSSs is essential in determining their physical parameters.

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DETECTION OF X-RAYS FROM THE SYMBIOTIC STAR V1329 Cyg

Cited by 10 publications

References 26 publications

Swiftobservations of the 2015 outburst of AG Peg – from slow nova to classical symbiotic outburst

Swiftobservations of the 2015 outburst of AG Peg – from slow nova to classical symbiotic outburst

Recent photometry of symbiotic stars

Multiwavelength modelling the SED of supersoft X-ray sources I. The method and examples

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