X-ray properties of symbiotic stars: I. The supersoft symbiotic novae RR tel and SMC3 (=RX J0048.4-7332)

Mürset, U.; Jordan, S.; Wolff, B.

doi:10.1007/bfb0102268

Cited by 69 publications

(121 citation statements)

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“…This spectrum is consistent with that of absorbed thermal plasma emission with emission detected up to ∼3 keV. Mürset et al (1997) and Luna et al (2013) classed the X-ray properties of Symbiotic binaries according to the nature and energetics of the spectrum. The integrated spectrum of AG Peg during outburst is similar, for instance, to Swift J1719-3002 made during a quiescent state ) which was classed as having a 'β' spectrum which indicates a spectrum peaking ∼0.8 keV, with most photons softer than 2.4 keV and is likely produced by a collision of winds from the white dwarf and red giant (∼1/3 of sources in the study of Luna et al show a β type spectrum).…”

Section: X-ray Spectrasupporting

confidence: 81%

“…Observations made using the Einstein and ROSAT satellites showed that symbiotic stars are X-ray emitters at relatively low flux levels when in a quiescent state (Allen 1981, Mürset, Wolff & Jordan 1997. Luna et al (2013) made a survey of symbiotic stars using the X-ray telescope (XRT) on-board the Swift satellite and found (as did Mürset et al 1997) that they could group the sources into those which c 0000 The Authors had very soft X-ray spectra (originating from shell burning on the surface of the white dwarf); those which had emission extending to ∼2.4 keV (probably due to the collision of winds from the red giant and white dwarf); and those which showed emission above ∼2.4 keV.…”

Section: Introductionmentioning

confidence: 99%

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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: X-ray Spectrasupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

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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“…Further investigation of AG Peg should include also its soft and super-soft X-ray domain as previously performed by Mürset et al (1997). The small value of the interstellar absorption to AG Peg and a very high level of its far-UV continuum, as measured by the FUSE and HST satellites, makes AG Peg a suitable target for detection of the supersoft X-rays.…”

Section: Ag Pegmentioning

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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“…Since AG Peg falls in the class β of the X-ray sources amongst symbiotic stars (showing emission form an optically thin plasma with a temperature of a few 10 6 K; Mürset et al 1997), the adopted spectral model was a sum of an absorbed optically thin plasma emission and a background component, as explained above. For the H, He, C and N abundances, we adopted the values derived by Schmutz (1996): H : He : C : N = 1 : 0.1 : 10 −5 : 10 −3 by number (H = 1, He = 1.02, C = 0.03, N = 8.93 with respect to the solar abundances; Anders & Grevesse 1989).…”

Section: Discrete-temperature Modelsmentioning

confidence: 99%

Recent X-ray observations of the symbiotic star AG Peg: do they signify colliding stellar winds?

Zhekov

Tomov

2016

Mon. Not. R. Astron. Soc.

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We present an analysis of recent X-ray observations of the symbiotic star AG Peg. The X-ray emission of AG Peg as observed with Swift in 2015 shows considerable variability on time scale of days as variability on shorter time scales might be present as well. Analysis of the X-ray spectra obtained in 2013 and 2015 confirms that AG Peg is an X-ray source of class β of the X-ray sources amongst the symbiotic stars. The X-ray emission of AG Peg as observed with ROSAT (1993 June) might well originate from colliding stellar winds (CSW) in binary system. On the other hand, the characteristics of the X-ray emission of AG Peg in 2013 and 2015 (Swift ) are hard to accommodate in the framework of the CSW picture. Analysis of the light curves in 2015 shows that the power spectrum of the X-ray variability in AG Peg resembles that of the flicker noise (or flickering) being typical for accretion processes in astronomical objects. This is a sign that CSWs did not play a key role for the X-ray emission from AG Peg in 2013-2015 and a different mechanism (probably accretion) is also getting into play.

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X-ray properties of symbiotic stars: I. The supersoft symbiotic novae RR tel and SMC3 (=RX J0048.4-7332)

Cited by 69 publications

References 10 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

Recent X-ray observations of the symbiotic star AG Peg: do they signify colliding stellar winds?

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