Low-frequency oscillations in black holes: a spectral-timing approach to the case of GX 339-4

Motta, S.; Muñoz-Darias, T.; Casella, P.; Belloni, T.; Homan, J.

doi:10.1111/j.1365-2966.2011.19566.x

Cited by 203 publications

(329 citation statements)

References 47 publications

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“…After that, the spectral parameters were compatible with the source changing from the LHS to the HIMS (until MJD ∼ 55303.6), then to softer states (to the SIMS until MJD 55304.7, then quickly to the SS, MJD ∼ 55306.1, and finally back to the SIMS and HIMS (see Fig. 3) around MJD 55320 (Motta et al 2010b), but this is beyond the scope of our paper because it happened after the observations listed in our Tables.…”

Section: X-ray and γ-Ray Spectramentioning

confidence: 81%

Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst

Bel

Rodríguez

D’Avanzo

et al. 2011

A&A

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Context. The microquasar GX 339−4 experienced a new outburst in 2010: it was observed simultaneously at various wavelengths from radio up to soft γ-rays. We focus on observations that are quasi-simultaneous with those made with the INTEGRAL and RXTE satellites: these were collected in 2010 March-April during our INTEGRAL target of opportunity programme, and during some of the other INTEGRAL observing programmes with GX 339−4 in the field-of-view. Aims. X-ray transients are extreme systems that often harbour a black hole, and are known to emit throughout the whole electromagnetic spectrum when in outburst. The goals of our programme are to understand the evolution of the physical processes close to the black hole and to study the connections between the accretion and ejection. Methods. We analysed radio, NIR, optical, UV, X-ray and soft γ-ray observations. We studied the source evolution in detail by producing light curves, hardness-intensity diagrams and spectra. We fitted the broadband data with phenomenological, then physical, models to study the emission coming from the distinct components. Results. Based on the energy spectra, the source evolved from the canonical hard state to the canonical soft state. The source showed X-ray spectral variations that were correlated with changes in radio, NIR and optical emission. The bolometric flux increased from 0.8 to 2.9 × 10 −8 erg cm −2 s −1 while the relative flux and contribution of the hot medium decreased on the average. Reprocessing in the disc was likely to be strong at the end of our observations. Conclusions. The source showed a behaviour similar to that of previous outbursts, with some small deviations in the hard X-ray parameter evolution. The radio, NIR and optical emission from jets was detected and observed to fade as the source softened. The results are discussed within the context of disc and jet models.

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Section: X-ray and γ-Ray Spectramentioning

confidence: 81%

Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst

Bel

Rodríguez

D’Avanzo

et al. 2011

A&A

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“…We find that the QPO frequency becomes ≈30% lower in accordance with the ≈20% decrease of the hard X-ray luminosity in the 15-50 keV band. LF QPOs (below 10 Hz) were detected in many BHXBs during the low/hard and intermediate states, such as XTE J150−564 (e.g., Cui et al 1999;Sobczak et al 1999) and GX 339−4 (e.g., Miyamoto et al 1991;Motta et al 2011;Tamura et al 2012). Previous studies suggested that their frequencies are positively correlated with the photon index of the Comptonization below ≈10 Hz, at which the correlation saturates (Vignarca et al 2003;Titarchuk & Fiorito 2004;Titarchuk & Shaposhnikov 2005).…”

Section: Origin Of Qpomentioning

confidence: 99%

SPECTRAL AND TIMING PROPERTIES OF THE BLACK HOLE X-RAY BINARY H1743–322 IN THE LOW/HARD STATE STUDIED WITHSUZAKU

Shidatsu

Ueda

Yamada

et al. 2014

ApJ

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We report on the results from Suzaku observations of the Galactic black hole X-ray binary H1743−322 in the low/hard state during its outburst in 2012 October. We appropriately take into account the effects of dust scattering to accurately analyze the X-ray spectra. The time-averaged spectra in the 1-200 keV band are dominated by a hard power-law component of a photon index of ≈1.6 with a high-energy cutoff at ≈60 keV, which is well described with the Comptonization of the disk emission by the hot corona. We estimate the inner disk radius from the multi-color disk component, and find that it is 1.3-2.3 times larger than the radius in the high/soft state. This suggests that the standard disk was not extended to the innermost stable circular orbit. A reflection component from the disk is detected with R = Ω/2π ≈ 0.6 (Ω is the solid angle). We also successfully estimate the stable disk component independent of the time-averaged spectral modeling by analyzing short-term spectral variability on a ∼1 s timescale. A weak low-frequency quasi-periodic oscillation at 0.1-0.2 Hz is detected, whose frequency is found to correlate with the X-ray luminosity and photon index. This result may be explained by the evolution of the disk truncation radius.

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“…The state is defined by changes in the PDS. The identifying feature is the presence of the so-called type-B QPO, which has been shown not to be an evolution of the one observed in the HIMS (type-C QPO; see Belloni et al 2005;Casella et al 2004Casella et al , 2005Motta et al 2011Motta et al , 2012. Notice that the SIMS in the HRD is characterised by a drop in total fractional rms (the ellipse in Fig.…”

Section: Soft Intermediate Statementioning

confidence: 99%

“…With the presence of a geometrically thick ADAF in the inner part of the flow, the PRCB can again operate efficiently in creating the magnetic field necessary for the production of a jet. The SIMS is entered again, as indicated by the appearance of type-B QPOs (Stiele et al 2011;Motta et al 2011).…”

Section: Soft Intermediate State At Low Luminositymentioning

confidence: 99%

Accretion and ejection in black-hole X-ray transients

Kylafis

Belloni

2015

A&A

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Context. A rich phenomenology has been accumulated over the years regarding accretion and ejection in black-hole X-ray transients (BHTs) and it needs an interpretation. Aims. Here we summarize the current observational picture of the outbursts of BHTs, based on the evolution traced in a hardnessluminosity diagram (HLD), and we offer a physical interpretation. Methods. The basic ingredient in our interpretation is the Poynting-Robertson cosmic battery (PRCB), which provides locally the poloidal magnetic field needed for the ejection of the jet. In addition, we make two assumptions, easily justifiable. The first is that the mass-accretion rate to the black hole in a BHT outburst has a generic bell-shaped form, whose characteristic time scale is much longer than the dynamical or the cooling ones. This is guaranteed by the observational fact that all BHTs start their outburst and end it at the quiescent state, i.e., at very low accretion rate, and that state transitions take place over long time scales (hours to days). The second assumption is that at low accretion rates the accretion flow is geometrically thick, ADAF-like, while at high accretion rates it is geometrically thin. Last, but not least, we demonstrate that the previous history of the system is absolutely necessary for the interpretation of the HLD. Results. Both, at the beginning and the end of an outburst, the PRCB establishes a strong poloidal magnetic field in the ADAF-like part of the accretion flow, and this explains naturally why a jet is always present in the right part of the HLD. In the left part of the HLD, the accretion flow is in the form of a thin disk, and such a disk cannot sustain a strong poloidal magnetic filed. Thus, no jet is expected in this part of the HLD. Finally, the counterclockwise traversal of the HLD is explained as follows: all outbursts start from the quiescent state, in which the inner part of the accretion flow is ADAF-like, threaded by a poloidal magnetic field. As the accretion rate increases and the source moves to the hard state, the poloidal magnetic field in the ADAF forces the flow to remain ADAF and the source to move upwards in the HLD rather than to turn left. Thus, the history of the system determines the counterclockwise traversal of the HLD. As a result, no BHT is expected to ever traverse the entire HLD curve in the clockwise direction. Conclusions. We offer a physical interpretation of accretion and ejection in BHTs with only one parameter, the mass transfer rate, plus the history of the system.

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Low-frequency oscillations in black holes: a spectral-timing approach to the case of GX 339-4

Cited by 203 publications

References 47 publications

Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst

Overview of an extensive multi-wavelength study of GX 339−4 during the 2010 outburst

SPECTRAL AND TIMING PROPERTIES OF THE BLACK HOLE X-RAY BINARY H1743–322 IN THE LOW/HARD STATE STUDIED WITHSUZAKU

Accretion and ejection in black-hole X-ray transients

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