ROSAT observations of symbiotic binaries and related objects

Bickert, K.; Greiner, J.; Stencel, R. E.

doi:10.1007/bfb0102267

Cited by 9 publications

(5 citation statements)

References 22 publications

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“…RX J0059.1-7505, the symbiotic star LIN 358 RX J0059.1−7505 was found by Mürset et al (1997) to be a SSS which coincides in position with the symbiotic SMC star LIN 358. X-ray emission of LIN 358 was also marginally detected by Bickert et al (1996) with a maximum likelihood ratio of 4.5 (≈2.5σ) in RASS data. RX J0059.1−7505 is classified in the catalog of Haberl et al (2000) as a SSS.…”

Section: Introductionmentioning

confidence: 94%

Supersoft sources inXMM-NewtonSmall Magellanic Cloud fields

Kahabka

Haberl

2006

A&A

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We report the detection and study of two faint ROSAT supersoft X-ray sources in the SMC field with XMM-Newton, RX J0059.1−7505 and RX J0059.4−7118. Due to the larger effective area of XMM-Newton we can constrain the X-ray spectra of both sources. RX J0059.1−7505 is optically identified with the symbiotic LIN 358 in the SMC. A ∼20 eV blackbody component dominates the observed spectrum. The soft blackbody component is consistent with steady nuclear burning in a shell although the spectrum is more complex than a simple blackbody continuum. RX J0059.4−7118 is not optically identified and we derive with the Optical Monitor (OM) a V magnitude > ∼ 19.3 assuming an M0 spectral type. The X-ray spectrum is fitted with a blackbody component with a temperature of ∼90 eV and an additional spectrally hard component which can be reproduced with a powerlaw. The luminosity of RX J0059.4−7118 would be ∼4 × 10 34 erg s −1 at the distance of the SMC. This is too large for a Cataclysmic Variable (CV). The spectral appearance is not in agreement with a supersoft source in the SMC. Thus we suggest that RX J0059.4−7118 is a Galactic source. As the optical magnitude derived from the OM data may be too faint for a normal Galactic CV we examined the possibility that RX J0059.4−7118 is a polar CV in the Galaxy, an isolated cooling neutron star (INS) at distance ∼(1−2) kpc, a pulsar with a brown dwarf companion, or a Galactic quiescent low-mass X-ray binary (qLMXB). We favor the hypothesis of a Galactic CV because of variability in the EPIC-pn data with a timescale of ∼1 h. A third supersoft ROSAT source, RX J0050.5−7455, is not detected with XMM-Newton.

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Section: Introductionmentioning

confidence: 94%

Supersoft sources inXMM-NewtonSmall Magellanic Cloud fields

Kahabka

Haberl

2006

A&A

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“…The star StHα 32 is a known supersoft source (Bickert et al 1996;Orio et al 2007) and it was included by accident in our target list. However, no X-ray spectrum has been published in the literature until now.…”

Section: Sthα 32mentioning

confidence: 99%

Symbiotic stars in X-rays

Luna

Sokoloski

Mukai

et al. 2013

A&A

122

175

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Until recently, symbiotic binary systems in which a white dwarf accretes from a red giant were thought to be mainly a soft X-ray population. Here we describe the detection with the X-ray Telescope (XRT) on the Swift satellite of nine white dwarf symbiotics that were not previously known to be X-ray sources and one that had previously been detected as a supersoft X-ray source. The nine new X-ray detections were the result of a survey of 41 symbiotic stars, and they increase the number of symbiotic stars known to be X-ray sources by approximately 30%. The Swift/XRT telescope detected all of the new X-ray sources at energies greater than 2 keV. Their X-ray spectra are consistent with thermal emission and fall naturally into three distinct groups. The first group contains those sources with a single, highly absorbed hard component that we identify as probably coming from an accretion-disk boundary layer. The second group is composed of those sources with a single, soft X-ray spectral component that probably originates in a region where low-velocity shocks produce X-ray emission, i.e., a colliding-wind region. The third group consists of those sources with both hard and soft X-ray spectral components. We also find that unlike in the optical, where rapid, stochastic brightness variations from the accretion disk typically are not seen, detectable UV flickering is a common property of symbiotic stars. Supporting our physical interpretation of the two X-ray spectral components, simultaneous Swift UV photometry shows that symbiotic stars with harder X-ray emission tend to have stronger UV flickering, which is usually associated with accretion through a disk. To place these new observations in the context of previous work on X-ray emission from symbiotic stars, we modified and extended the α/β/γ classification scheme for symbiotic-star X-ray spectra that was introduced by Muerset et al. based upon observations with the ROSAT satellite, to include a new δ classification for sources with hard X-ray emission from the innermost accretion region. Because we have identified the elusive accretion component in the emission from a sample of symbiotic stars, our results have implications for the understanding of wind-fed mass transfer in wide binaries, and the accretion rate in one class of candidate progenitors of type Ia supernovae.

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“…Plus (+) means a detection; minus (−) means that an object was observed but not detected and that only an upper limit is available. Most of the detections and upper limits came from ROSAT and were reported in [35] but some have also been observed by Einstein [15], EXOSAT and ASCA.…”

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confidence: 94%

“…[198,237] (optical spectra), [303,111] (emission line profiles and radial velocity measurements) [233] (optical and IR photometry), [142,315] (IRAS observations), [280,279,278,112,117] (radio emission), [116,274] (searches for maser emission), [187] (IUE observations), [35,238] (X-ray emission), [312] (symbiotic miras), [235] (symbiotic novae), [236,215] (extragalactic symbiotics) and in-depth investigations, e.g. [109,205,110,287,83] for AX Per alone.…”

Section: Introductionmentioning

confidence: 99%

A catalogue of symbiotic stars

Belczyński

Mikołajewska

Munari

et al. 2000

Astron. Astrophys. Suppl. Ser.

379

407

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Abstract. We present a new catalogue of symbiotic stars. In our list we include 188 symbiotic stars as well as 30 objects suspected of being symbiotic. For each star, we present basic observational material: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radio observations. We also list the spectral type of the cool component, the maximum ionization potential observed, references to finding charts, spectra, classifications and recent papers discussing the physical parameters and nature of each object. Moreover, we present the orbital photometric ephemerides and orbital elements of known symbiotic binaries, pulsational periods for symbiotic Miras, Hipparcos parallaxes and information about outbursts and flickering.

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ROSAT observations of symbiotic binaries and related objects

Cited by 9 publications

References 22 publications

Supersoft sources inXMM-NewtonSmall Magellanic Cloud fields

Supersoft sources inXMM-NewtonSmall Magellanic Cloud fields

Symbiotic stars in X-rays

A catalogue of symbiotic stars

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