A jet model for Galactic black-hole X-ray sources: The correlation between cutoff energy and phase lag

Reig, P.; Kylafis, N. D.

doi:10.1051/0004-6361/201527151

Cited by 28 publications

(40 citation statements)

References 35 publications

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“…Over the years we have developed a jet model to explain the spectral and timing properties of BHBs (Reig et al 2003;Giannios et al 2004;Giannios 2005;Kylafis et al 2008;Reig & Kylafis 2015).…”

Section: A Jet Modelmentioning

confidence: 99%

“…The difference can be attributed to the acceleration region, which was absent in Kylafis et al (2008). The acceleration zone was introduced to explain the correlation between the cut-off energy and phase lags in GX 339-4 (Reig & Kylafis 2015). As shown in Reig & Kylafis (2015), for a given value of τ , the models with the acceleration zone produce shorter lags than when acceleration occurs instantaneously.…”

Section: A Jet Modelmentioning

confidence: 99%

“…The acceleration zone was introduced to explain the correlation between the cut-off energy and phase lags in GX 339-4 (Reig & Kylafis 2015). As shown in Reig & Kylafis (2015), for a given value of τ , the models with the acceleration zone produce shorter lags than when acceleration occurs instantaneously. The natural way to increase the lags is by increasing the size of the jet.…”

Section: A Jet Modelmentioning

confidence: 99%

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The photon-index–time-lag correlation in black hole X-ray binaries

Reig

Kylafis

Papadakis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We have performed a timing and spectral analysis of a set of black-hole binaries to study the correlation between the photon index and the time lag of the hard photons with respect to the soft ones. We provide further evidence that the timing and spectral properties in black-hole X-ray binaries are coupled. In particular, we find that the average time lag increases as the X-ray emission becomes softer. Although a correlation between the hardness of the X-ray spectrum and the time (or phase) lag has been reported in the past for a handful of systems, our study confirms that this correlated behaviour is a global property of black-hole X-ray binaries. We also demonstrate that the photon-index -time-lag correlation can be explained as a result of inverse Comptonization in a jet.

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Section: A Jet Modelmentioning

confidence: 99%

Section: A Jet Modelmentioning

confidence: 99%

Section: A Jet Modelmentioning

confidence: 99%

See 1 more Smart Citation

The photon-index–time-lag correlation in black hole X-ray binaries

Reig

Kylafis

Papadakis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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show abstract

“…The model that we have used in this work is identical to that used in Reig & Kylafis (2015). For our Monte Carlo code we follow Pozdnyakov et al (1983).…”

Section: The Modelmentioning

confidence: 99%

“…In a series of papers (Reig et al 2003;Giannios et al 2004;Giannios 2005;Kylafis et al 2008;Reig & Kylafis 2015), we showed that Compton upscattering of soft photons from the accretion disk in the jet can explain a number of observational relations between the spectral and timing parameters in the hard state of BHXB. Our results clearly demonstrate that jets play a central role in all the observed phenomena, not only in the radio emission.…”

Section: Introductionmentioning

confidence: 99%

The origin of the hard X-ray tail in neutron-star X-ray binaries

Reig

Kylafis

2016

A&A

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Context. Neutron star X-ray binaries emit a compact, optically thick, relativistic radio jet during low-luminosity, usually hard states, as Galactic black-hole X-ray binaries do. When radio emission is bright, a hard power-law tail without evidence for an exponential cutoff is observed in most systems. Aims. We have developed a jet model that explains many spectral and timing properties of black-hole binaries in the states where a jet is present. Our goal is to investigate whether our jet model can reproduce the hard tail, with the correct range of photon index and the absence of a high-energy cutoff, in neutron-star X-ray binaries. Methods. We performed Monte Carlo simulations of the Compton upscattering of soft, accretion-disk or boundary layer photons in the jet and computed the emergent energy spectra, as well as the time lag of hard photons with respect to softer ones as a function of Fourier frequency. We fit the energy spectra with a power law modified by an exponential cutoff at high energy. Results. We demonstrate that our jet model naturally explains the observed power-law distribution with photon index in the range 1.8-3. With an appropriate choice of the parameters, the cutoff expected from Comptonization is shifted to energies above ∼300 keV, producing a pure power law without any evidence for a rollover, in agreement with the observations. Conclusions. Our results reinforce the idea that the link between the outflow (jet) and inflow (disk) in X-ray binaries does not depend on the nature of the compact object, but on the process of accretion. Furthermore, we address the differences between jets in black-hole and neutron-star X-ray binaries and predict that the break frequency in the spectral energy distribution of neutron-star X-ray binaries, as a class, will be lower than that of black-hole binaries.

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The X-ray view of black-hole candidateSwiftJ1842.5-1124 during its 2008 outburst

Zhao

Weng

et al. 2016

A&A

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Context. The spectral and temporal evolution during X-ray outbursts give important clues on the accretion process and radiation mechanism in black-hole X-ray binaries (BH XRBs). Aims. A set of Swift and RXTE observations were executed to monitor the 2008 outburst of the black-hole candidate Swift J1842.5-1124. We investigate these data to explore the accretion physics in BH XRBs. Methods. We carry out a comprehensive spectral and timing analysis on all the available pointing observations, including fitting both X-ray spectra and power density spectra, measuring the optical and near-ultraviolet flux density. We also search for correlations among the spectral and timing parameters. Results. The observed properties of Swift J1842.5-1124 are similar to other BH XRBs in many respects, for example the hardnessintensity diagram and hardness-rms diagram. The type-C quasi-periodic oscillations (QPOs) were observed as the source started to transit from the low-hard state to the high-soft state. The frequency of QPOs correlate with intensity and the hard component index, and anti-correlate with the hardness and the total fractional rms. These relations are consistent with the Lense-Thirring precession model. The estimated U-band flux changed with the X-ray flux, while the flux density at the V band remained 0.26 mJy. These results imply that the X-ray reprocessing or the tail of thermal emission from the outer disk contributes a significant fraction of the U-band radiation; alternatively, the companion star or the jet dominates the flux at longer wavelengths.

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A jet model for Galactic black-hole X-ray sources: The correlation between cutoff energy and phase lag

Cited by 28 publications

References 35 publications

The photon-index–time-lag correlation in black hole X-ray binaries

The photon-index–time-lag correlation in black hole X-ray binaries

The origin of the hard X-ray tail in neutron-star X-ray binaries

The X-ray view of black-hole candidateSwiftJ1842.5-1124 during its 2008 outburst

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