<i>ASCA</i>Observations of GX 354−0 and KS 1731−260

Narita, T.; Grindlay, J.; Barret, D.

doi:10.1086/318326

Cited by 26 publications

(30 citation statements)

References 24 publications

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“…We conclude that the persistent X-ray spectra days to weeks after the flare (when no normal bursts occurred) are not different from the spectra days to weeks before 3 Previously, a black-body component (or a disk black-body component) has been included in spectral fits (Barret et al 2000;Narita et al 2001). We, however, found their inclusion made the fits rather unstable, while providing little (spectra A and F) or no (B-E) improvement.…”

Section: Persistent Emissionmentioning

confidence: 71%

A half-a-day long thermonuclear X-ray burst from KS 1731-260

Kuulkers

Zand

Kerkwijk

et al. 2002

A&A

116

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Abstract.We report on an approximately twelve hour long X-ray flare from the low-mass X-ray binary KS 1731−260. The flare has a rise time of less than 13 min and declines exponentially with a decay time of 2.7 hours. The flare emission is well described by black-body radiation with peak temperature of 2.4 keV. The total energy release from the event is 10 42 erg (for an assumed distance of 7 kpc). The flare has all the characteristics of thermo-nuclear X-ray bursts (so-called type I X-ray bursts), except for its very long duration and therefore large energy release (factor of 1500-4000 longer and 250-425 more energy than normal type I X-ray bursts from this source). The flare is preceded by a short and weak X-ray burst, possibly of type I. Days to weeks before the flare, type I X-ray bursts were seen at a rate of ∼3 per day. However, after the flare type I X-ray bursting ceased for at least a month, suggesting that the X-ray flare affected the type I bursting behaviour. The persistent emission is not significantly different during the non-bursting period. We compare the characteristics of this event with similar long X-ray flares, so-called superbursts, seen in other sources (4U 1735−44, 4U 1820−30, 4U 1636−53, Ser X-1, GX 3+1). The event seen from KS 1731−260 is the longest reported so far. We discuss two possible mechanisms that might cause these superbursts, unstable carbon burning (as proposed recently) and electron capture by protons with subsequent capture of the resulting neutrons by heavy nuclei.

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Section: Persistent Emissionmentioning

confidence: 71%

A half-a-day long thermonuclear X-ray burst from KS 1731-260

Kuulkers

Zand

Kerkwijk

et al. 2002

A&A

116

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“…Spectral analysis of MXB 1728-34 has been performed in the past using data from different satellites, such as Einstein (Grindlay & Hertz 1981), SAS-3 (Basinska et al 1984), EXOSAT (White et al 1986), SIGMA (Claret et al 1994), ROSAT (Schulz 1999), and more recently using BeppoSAX (Piraino et al 2000;Di Salvo et al 2000), ASCA (Narita et al 2001), RXTE, Chandra (D'Aì et al 2006, INTEGRAL (Falanga et al 2006), and XMM-Newton (Ng et al 2010). The X-ray spectrum is generally composed of a soft and a hard component.…”

Section: Introductionmentioning

confidence: 99%

X-ray spectroscopy of MXB 1728–34 withXMM-Newton

Egron

Salvo

Burderi

et al. 2011

A&A

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We analyzed an XMM-Newton observation of the low-mass X-ray binary and atoll source MXB 1728-34. The source was in a lowluminosity state during the XMM-Newton observation, corresponding to a bolometric X-ray luminosity of 5 × 10 36 d 2 5.1 kpc erg s −1 . The 1-11 keV X-ray spectrum of the source, obtained combining data from all the five instruments on-board XMM-Newton, is well fitted by a Comptonized continuum. Evident residuals are present at 6−7 keV, which are ascribed to the presence of a broad iron emission line. This feature can be equally well fitted by a relativistically smeared line or by a self-consistent, relativistically smeared reflection model. Under the hypothesis that the iron line is produced by reflection from the inner accretion disk, we can infer important information on the physical parameters of the system, such as the inner disk radius, R in = 25−100 km, and the inclination of the system, 44• < i < 60• .

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“…Since its discovery the source was extensively observed by various X-ray observatories (e.g. Barret et al 1993;Barret et al 1998;Smith et al 1997;Narita et al 2001).…”

Section: Introductionmentioning

confidence: 99%

A possible 38 day X-ray period of KS 1731-260

Revnivtsev

Sunyaev

2003

A&A

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Abstract. We report the detection of a 38 day period of the X-ray transient and X-ray burster KS 1731-260. The periodicity was detected during Mar.1996-Aug.1998 when the source had a high and relatively stable X-ray flux. After Sep.-Oct. 1998 (∼TJD 11100) the source became strongly variable on a time scale of months that contaminates the search for the 38 day periodicity. The detected period can not be a binary period. A binary with Roche lobe overflow has in this case large radii of the secondary and of the accretion disk. Illumination of the disk and secondary star by the X-ray flux from the luminous neutron star and inner disk, would lead to a high infrared brightness of the binary. That clearly contradicts the infrared data even for the brightest infrared sources within CHANDRA error box of KS 1731-260. A remaining possibility is that observed periodicity is connected with the accretion disk precession, similar to that was observed for, e.g. SS 433 and Her X-1.

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ASCAObservations of GX 354−0 and KS 1731−260

Cited by 26 publications

References 24 publications

A half-a-day long thermonuclear X-ray burst from KS 1731-260

A half-a-day long thermonuclear X-ray burst from KS 1731-260

X-ray spectroscopy of MXB 1728–34 withXMM-Newton

A possible 38 day X-ray period of KS 1731-260

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