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

Belloni, T.; Homan, J.; Casella, P.; Klis, M. van der; Nespoli, E.; Lewin, W. H. G.; Miller, J. M.; Méndez, Mariano

doi:10.1051/0004-6361:20042457

Cited by 503 publications

(757 citation statements)

References 57 publications

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“…Various spectral states were identified during different phases of the outburst. In general, four basic spectral states (Hard, Hard − Intermediate, S o f t − Intermediate, S o f t) are observed during the outburst of a transient BHC Belloni et al, 2005;Nandi et al, 2012). One can find After almost two decades, in 2003, the INTEGRAL satellite discovered signatures of renewed activity in hard X-rays (Revnivtsev et al, 2003) and later, RXTE also verified the presence of such an activity (Markwardt & Swank, 2003).…”

Section: Introductionmentioning

confidence: 99%

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Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

Debnath

Chakrabarti

Nandi

2013

Advances in Space Research

111

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The Galactic black hole candidate H 1743-322 exhibited two X-ray outbursts in rapid succession: one in August 2010 and the other in April 2011. We analyze archival data of this object from the PCA instrument on board RXTE (2-25 keV energy band) to study the evolution of its temporal and spectral characteristics during both the outbursts, and hence to understand the behavioral change of the accretion flow dynamics associated with the evolution of the various X-ray features. We study the evolution of QPO frequencies during the rising and the declining phases of both the outbursts. We successfully fit the variation of QPO frequency using the Propagating Oscillatory Shock (POS) model in each of the outbursts and obtain the accretion flow parameters such as the instantaneous shock locations, the shock velocity and the shock strength. Based on the degree of importance of the thermal (disk black body) and the non-thermal (power-law) components of the spectral fit and properties of the QPO (if present), the entire profiles of the 2010 and 2011 outbursts are subdivided into four different spectral states: hard, hard-intermediate, soft-intermediate and soft. We attempt to explain the nature of the outburst profile (i.e., hardness-intensity diagram) with two different types of mass accretion flow.

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Section: Introductionmentioning

confidence: 99%

“…Several attempts Belloni et al, 2005;Nandi et al, 2012) were made for a thorough study on the temporal and spectral evolutions of the transient black hole (BH) binaries during their outbursts. Various spectral states were identified during different phases of the outburst.…”

Section: Introductionmentioning

confidence: 99%

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

Debnath

Chakrabarti

Nandi

2013

Advances in Space Research

111

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“…in the typical frequency range ∼ 0.1 − 60 Hz) aperiodic variability progressively decreases as the outburst evolves, with the fractional root-mean-square (rms) variability amplitude (e.g. Nandra et al 1997;Vaughan et al 2003; ⋆ E-mail: bdemarco@mpe.mpg.de Ponti et al 2004) dropping from values of tens of percent in the canonical hard state, down to a few percent in the canonical soft state (Belloni et al 2005; Muñoz-Darias, . During the hard state the fractional rms shows an "inverted spectrum" (decreasing with energy), which switches to a "hard spectrum" (increasing with energy, at least above ∼5 keV) during intermediate and soft states (e.g.…”

Section: Introductionmentioning

confidence: 99%

The evolution of the disc variability along the hard state of the black hole transient GX 339-4

Marco¹,

Ponti²,

Muñoz-Darias³

et al. 2015

Mon. Not. R. Astron. Soc.

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We report on the analysis of hard-state power spectral density function (PSD) of GX 339-4 down to the soft X-ray band, where the disc significantly contributes to the total emission. At any luminosity probed, the disc in the hard state is intrinsically more variable than in the soft state. However, the fast decrease of disc variability as a function of luminosity, combined with the increase of disc intensity, causes a net drop of fractional variability at high luminosities and low energies, which reminds the well-known behaviour of disc-dominated energy bands in the soft state. The peak-frequency of the high-frequency Lorentzian (likely corresponding to the high-frequency break seen in active galactic nuclei, AGN) scales with luminosity, but we do not find evidence for a linear scaling. In addition, we observe that this characteristic frequency is energy-dependent. We find that the normalization of the PSD at the peak of the high-frequency Lorentzian decreases with luminosity at all energies, though in the soft band this trend is steeper. Together with the frequency shift, this yields quasi-constant high frequency (5-20 Hz) fractional rms at high energies, with less than 10 percent scatter. This reinforces previous claims suggesting that the high frequency PSD solely scales with BH mass. On the other hand, this constancy breaks down in the soft band (where the scatter increases to ∼ 30 percent). This is a consequence of the additional contribution from the disc component, and resembles the behaviour of optical variability in AGN.

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“…1 the evolution of the prototypical transient GX 339-4 during an outburst is sketched in the hardnessintensity plane (harder spectra correspond to points on the right). As the outburst proceeds, the diagram is followed counter-clockwise and the source passes through the different states (Homan & Belloni 2005;Belloni et al 2005). The line whose crossing corresponds to the jet ejection is the dotted line at the top, also called "jet line" (Fender, Belloni & Gallo 2004).…”

Section: Jets In X-ray Binariesmentioning

confidence: 99%

Relativistic Jets from Active Galactic Nuclei

Böttcher¹,

Harris²,

Krawczynski³

2012

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Abstract. Relativistic jets from Active Galactic Nuclei are known since decades, but the study of the connection between accretion and ejection in these systems is hampered by the long time scales associated to these events. The past decade has seen a rapid advancement due to the observation of similar radio jets in galactic X-ray binaries, where the time scales are much shorter. A clear connection between accretion and ejection has been found for these systems, together with a solid characterization of the phenomenological properties of their outbursts. This wealth of new results has led to a detailed comparison between X-ray binaries and AGN, from which a number of correlations and scaling laws has been established. Here I briefly review the current observational status.

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

Cited by 503 publications

References 57 publications

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

The evolution of the disc variability along the hard state of the black hole transient GX 339-4

Relativistic Jets from Active Galactic Nuclei

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