The X-ray spectrum of the black hole candidate GX339-4 in a low state

Corongiu, A.; Chiappetti, L.; Haardt, Francesco; Treves, A.; Colpi, M.; Belloni, T.

doi:10.1051/0004-6361:20030923

Cited by 10 publications

(14 citation statements)

References 28 publications

(62 reference statements)

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“…We note that the relatively strong Compton reflection measured in X‐ray spectra of GX 339−4 (e.g. Z98; W02; Corongiu et al 2003) appears incompatible with i ≃ 80°; however, an investigation of this issue is beyond the scope of this paper.…”

Section: The Distance To Gx 339−4mentioning

confidence: 86%

“…We have assumed that there is a constant total power in the soft blackbody spectrum, but its fraction irradiating the hot plasma is variable, as discussed above. We assumed the soft photon spectrum is a disc blackbody with the maximum temperature of kT bb = 0.4 keV (Corongiu et al 2003), and τ= 2 (W02).…”

Section: Discussion and Theoretical Interpretationmentioning

confidence: 99%

“…These differentiae are likely to be related to the T bb in the hard state being much higher in GX 339−4 than in Cyg X‐1. Indeed, Corongiu et al (2003) obtain T bb ∼ 0.4 keV in the hard state of GX 339−4, compared to ∼ 0.15 keV in Cyg X‐1 (Di Salvo et al 2001; Frontera 2001). 1 Then, the variability pattern of the blackbody emission (see ) affects the ASM band much more in GX 339−4 than in Cyg X‐1. The hard‐state fluxes in bands from 20 to 160 keV are positively correlated with the local spectral indices in GX 339−4.…”

Section: Comparison With Cyg X‐1mentioning

confidence: 95%

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GX 339−4: the distance, state transitions, hysteresis and spectral correlations

Zdziarski

Gierliński

Mikołajewska

et al. 2004

Monthly Notices of the Royal Astronomical Society

281

309

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We study the X‐ray variability and distance of GX 339−4. We derive the distance of ≳7 kpc, based on a recent determination of the binary parameters. We study data from the All‐Sky Monitor (ASM) aboard Ginga, the Burst and Transient Source Experiment aboard the Compton Gamma Ray Observatory, and the ASM, Proportional Counter Array and High‐Energy Transient X‐ray Experiment aboard the Rossi X‐ray Timing Explorer (RXTE). From 1987 to 2004, GX 339−4 underwent ∼15 outbursts and went through all known states of black hole binaries. For the first time, we present the PCA data from the initial hard state of the outburst of 2004. We then study colour–colour and colour–flux correlations. In the hard state, there is a strong anticorrelation between the 1.5–5 and 3–12 keV spectral slopes, which we explain by thermal Comptonization of disc photons. There is also a softening of the spectrum above 3 keV with the increasing flux that becomes stronger with increasing energy up to ∼200 keV. This indicates an anticorrelation between the electron temperature and luminosity, explained by hot accretion models. In addition, we see a variable broad‐band slope with a pivot at ∼200 keV. In the soft state, there is a high‐energy tail with varying amplitude beyond a strong and variable blackbody component. We confirm the presence of pronounced hysteresis, with the hard‐to‐soft state transitions occurring at much higher (and variable) luminosities than the soft‐to‐hard transitions. We fitted the RXTE/ASM data with a model consisting of an outer accretion disc and a hot inner flow. State transitions are associated then with variations in the disc truncation radius, which we fitted as ∼6GM/c2 in the soft state and several times that in the hard state. The disappearance of the inner disc takes place at a lower accretion rate than its initial appearance owing to the dependence of the transitions on the source history. We provide further evidence against the X‐ray emission in the hard state being non‐thermal synchrotron, and explain the observed radio–X‐ray correlation by the jet power being correlated with the accretion power.

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Section: The Distance To Gx 339−4mentioning

confidence: 86%

Section: Discussion and Theoretical Interpretationmentioning

confidence: 99%

Section: Comparison With Cyg X‐1mentioning

confidence: 95%

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GX 339−4: the distance, state transitions, hysteresis and spectral correlations

Zdziarski

Gierliński

Mikołajewska

et al. 2004

Monthly Notices of the Royal Astronomical Society

281

309

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“…The system was one of the two that showed all "canonical" X-ray states of BHCs (LS, HS and VHS: see Miyamoto et al 1991). From the launch of the Rossi X-Ray Timing Explorer (RXTE) until 1999 it remained bright, mostly in the Low/Hard state but with a transition to a softer state (see Nowak et al 1999;Wilms et al 1999;Belloni et al 1999;Nowak et al 2002;Corongiu et al 2003). In 1999, the source went into quiescence, where it was detected with BeppoSAX at low flux levels (Kong et al 2000;Corbel et al 2003).…”

Section: Introductionmentioning

confidence: 99%

The evolution of the timing properties of the black-hole transient GX 339–4 during its 2002/2003 outburst

Belloni¹,

Homan

Casella

et al. 2005

A&A

Self Cite

494

684

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Abstract. We present the results of the timing and color analysis of more than two hundred RXTE/PCA observations of the bright black-hole transient GX 339-4 obtained during its 2002/2003 outburst. The color-intensity evolution of the system, coupled to the properties of its fast time variability, allow the identification of four separate states. Depending on the state, strong noise is detected, together with a variety of quasi-periodic oscillations at frequencies from 0.2 to 8 Hz. We present a characterization of the timing parameters of these states and compare them to what has been observed in other systems. These results, together with those obtained from energy spectra, point towards a common evolution of black-hole transients through their outbursts.

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“…The disk+corona models with different geometries, such as, an accretion disk corona (ADC) above or surrounded by a cold thin disk, or other similar geometries (see Nowak et al 2002, for de-tails and references therein), are used to interpret the observational features of the accretion flows around the black hole in different states. The observed X-ray spectra in different spectral states can be explained by the Comptonization ( e.g., soft photons from the cold thin accretion disk are Comptonized in a hot corona) with different model parameters (Nowak et al 2002;Corongiu et al 2003). Narayan (1996) proposed that these different spectral states can be explained by outer thin disk plus inner advection dominated accretion flow (ADAF) models with varying accretion rate and transition radius (Esin et al 1997(Esin et al , 1998.…”

Section: Introductionmentioning

confidence: 99%

Thermal X-Ray Iron Line Emission From the Advection-Dominated Accretion Flow in the Galactic Binary Gx 339–4

2011

ApJ

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We explore thermal X-ray iron line emission from the galactic X-ray binary GX 339-4 in the off state, using the models of the advection dominated accretion flow (ADAF) without or with outflows. The equivalent widths of hydrogen-like and helium-like thermal iron lines are calculated with different model parameters including viscosity parameter α, mass accretion rate at the outer radius of the ADAFṁ out and outflow strength parameter p. Our calculations show that the equivalent widths of thermal iron lines emitted from the pure ADAF, i.e., the ADAF without outflows, should be very small, assuming a solar metallicity for the accreting gas in the accretion flow. Strong thermal iron lines are expected to be emitted from the ADAF with relatively strong outflows. For reasonable choice of parameters, the total equivalent width of the He-like and H-like thermal iron lines reaches to 500 eV for accreting gas with solar metallicity. The observation of strong thermal X-ray lines from GX 339-4 at the off state may give a clue to the accretion mode of the source and provide evidence for the presence of outflows/winds in the accretion flow around the black hole in GX 339-4. It is found that the values ofṁ out and p are degenerate, i.e., the observed X-ray continuum spectrum can be fairly well reproduced with different sets of the parametersṁ out and p. Such degeneracy can be broken when the thermal X-ray line emission data is available. We also compare our results with those in the previous similar work.

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The X-ray spectrum of the black hole candidate GX339-4 in a low state

Cited by 10 publications

References 28 publications

GX 339−4: the distance, state transitions, hysteresis and spectral correlations

GX 339−4: the distance, state transitions, hysteresis and spectral correlations

The evolution of the timing properties of the black-hole transient GX 339–4 during its 2002/2003 outburst

Thermal X-Ray Iron Line Emission From the Advection-Dominated Accretion Flow in the Galactic Binary Gx 339–4

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