Quasi-periodic oscillations in the Z source GX 340 + 0

Penninx, W.; Lewin, W. H. G.; Tan, J.; Mitsuda, Kazuhisa; Klis, M. van der; Paradijs, J. van

doi:10.1093/mnras/249.1.113

Cited by 22 publications

(34 citation statements)

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“…Both sources trace out a clear Z track and an extra branch is available at the end of the FB. Such behavior has already been reported before in GX 5−1 [10] and GX 340+0 [11].…”

Section: Resultssupporting

confidence: 87%

KiloHertz quasi-periodic oscillations in the Z sources GX 340+0, Cygnus X-2, GX 17+2, GX 5–1, and Scorpius X-1

Wijnands

Klis

1998

AIP Conference Proceedings

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Abstract.We have discovered kiloHertz quasi-periodic oscillations (kHz QPOs) in five Z sources: GX 340+0, Cygnus X-2, GX 17+2, GX 5−1, and Scorpius X-1. In all sources the properties of these kHz QPOs are very similar and closely related to the position of the sources on the Z track traced out in the X-ray color-color diagram and the hardness-intensity diagram. The frequencies of the kHz QPOs increase when the sources move from the left end of the horizontal branch to horizontal/normal branch vertex, thus with inferred mass accretion rate. Only for Scorpius X-1 the kHz QPOs have been observed down the normal branch unto the flaring branch. The strength and the FWHM of the higherfrequency kHz QPOs decrease with mass accretion rate, but when the lowerfrequency kHz QPOs are detected the strength and the FWHM of this QPO stay approximately constant with mass accretion rate. In Scorpius X-1 the frequency separation between the kHz QPOs decreases with mass accretion rate, but in the other Z sources the separation remains approximately constant, although a similar decrease in peak separation as found in Scorpius X-1 can not be excluded.

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“…Both sources trace out a clear Z track and an extra branch is available at the end of the FB. Such behavior has already been reported before in GX 5−1 [10] and GX 340+0 [11].…”

Section: Resultssupporting

confidence: 87%

KiloHertz quasi-periodic oscillations in the Z sources GX 340+0, Cygnus X-2, GX 17+2, GX 5–1, and Scorpius X-1

Wijnands

Klis

1998

AIP Conference Proceedings

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“…Another peak appears in PDS‐V: its centroid frequency correlates with the count rate and its quality factor Q is ∼2: we identify this peak as a HBO. HBOs on the NB have already been detected in other Z sources (GX 340+0, Penninx et al 1991; GX 17+2, Wijnands et al 1996; Homan et al 2002; Cyg X‐2, Wijnands et al 1997; GX 5‐1, Dotani 1988) but they have never been clearly detected in Cir X‐1.…”

Section: Results and Interpretationmentioning

confidence: 99%

Linking jet emission and X-ray properties in the peculiar neutron star X-ray binary Circinus X-1

Soleri

Tudose

Fender

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We present the results of simultaneous X‐ray and radio observations of the peculiar Z‐type neutron star X‐ray binary Cir X‐1, observed with the Rossi X‐ray Timing Explorer satellite and the Australia Telescope Compact Array in 2000 October and 2002 December. We identify typical Z‐source behaviour in the power density spectra as well as characteristic Z patterns drawn in an X‐ray hardness–intensity diagram. Power spectra typical of bright atoll sources have also been identified at orbital phases after the periastron passage, while orbital phases before the periastron passage are characterized by power spectra that are typical neither of Z nor of atoll sources. We investigate the coupling between the X‐ray and the radio properties, focusing on three orbital phases when an enhancement of the radio flux density has been detected, to test the link between the inflow (X‐ray) and the outflow (radio jet) to/from the compact object. In two out of three cases, we associate the presence of the radio jet to a spectral transition in the X‐rays, although the transition does not precede the radio flare, as detected in other Z sources. An analogous behaviour has recently been found in the black hole candidate GX 339‐4. In the third case, the radio light curve shows a similar shape to the X‐ray light curve. We discuss our results in the context of jet models, considering also black hole candidates.

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“…The source was classified as a Z-track source by Hasinger & van der Klis (1989). QPO were found in Exosat data (van Paradijs et al 1988) and in Ginga data (Penninx et al 1991) and kilohertz QPO were discovered by Jonker et al (1998). The detection of radio by Penninx et al (1993) is important indicating the presence of jets.…”

Section: Approach Of the Present Workmentioning

confidence: 93%

An explanation of the Z-track sources

Church

Halai²,

Bałucińska‐Church

2006

A&A

101

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We present an explanation of the Z-track phenomenon based on spectral fitting results of Rossi-XTE observations of the source GX 340+0 using the emission model previously shown to describe the dipping Low Mass X-ray Binaries. In our Z-track model, the soft apex is a quiescent state of the source with lowest luminosity. Moving away from this point by ascending the normal branch the strongly increasing luminosity of the Accretion Disc Corona (ADC) Comptonized emission L ADC provides substantial evidence for a large increase of mass accretion rateṀ. There are major changes in the neutron star blackbody emission, kT increasing to high values, the blackbody radius R BB decreasing, these changes continuing monotonically on both normal and horizontal branches. The blackbody flux increases by a factor of ten to three times the Eddington flux so that the physics of the horizontal branch is dominated by the high radiation pressure of the neutron star, which we propose disrupts the inner disc, and an increase of column density is detected. We further propose that the very strong radiation pressure is responsible for the launching of the jets detected in radio on the horizontal branch. On the flaring branch, we find that L ADC is constant, suggesting no change inṀ so that flaring must consist of unstable nuclear burning. At the soft apex, the mass accretion rate per unit area on the neutron starṁ is minimum for the horizontal and normal branches and about equal to the theoretical upper limit for unstable burning. Thus it is possible that unstable burning begins as soon as the source arrives at this position, the onset of unstable burning being consistent with theory. The large increase in R BB in flaring is reminiscent of radius expansion in X-ray bursts. Finally, in our model,Ṁ does not increase monotonically along the Z-track as often previously thought.

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Quasi-periodic oscillations in the Z source GX 340 + 0

Cited by 22 publications

References 0 publications

KiloHertz quasi-periodic oscillations in the Z sources GX 340+0, Cygnus X-2, GX 17+2, GX 5–1, and Scorpius X-1

KiloHertz quasi-periodic oscillations in the Z sources GX 340+0, Cygnus X-2, GX 17+2, GX 5–1, and Scorpius X-1

Linking jet emission and X-ray properties in the peculiar neutron star X-ray binary Circinus X-1

An explanation of the Z-track sources

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