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Modelling Spectral and Timing Properties of Accreting Black Holes: The Hybrid Hot Flow Paradigm

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Abstract

The general picture that emerged by the end of 1990s from a large set of optical and X-ray, spectral and timing data was that the X-rays are produced in the innermost hot part of the accretion flow, while the optical/infrared (OIR) emission is mainly produced by the irradiated outer thin accretion disc. Recent multiwavelength observations of Galactic black hole transients show that the situation is not so simple. Fast variability in the OIR band, OIR excesses above the thermal emission and a complicated interplay between the X-ray and the OIR light curves imply that the OIR emitting region is much more compact. One of the popular hypotheses is that the jet contributes to the OIR emission and even is responsible for the bulk of the X-rays. However, this scenario is largely ad hoc and is in contradiction with many previously established facts. Alternatively, the hot accretion flow, known to be consistent with the X-ray spectral and timing data, is also a viable candidate to produce the OIR radiation. The hot-flow scenario naturally explains the power-law like OIR spectra, fast OIR variability and its complex relation to the X-rays if the hot flow contains non-thermal electrons (even in energetically negligible quantities), which are required by the presence of the MeV tail in Cyg X-1. The presence of non-thermal electrons also lowers the equilibrium electron temperature in the hot flow model to ≲100 keV, making it more consistent with observations. Here we argue that any viable model should simultaneously explain a large set of spectral and timing data and show that the hybrid (thermal/non-thermal) hot flow model satisfies most of the constraints.

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Notes

  1. Note that the electron temperature can be measured only if high-quality data are available above 100 keV and accurate Comptonization models such as compps (Poutanen and Svensson 1996) or eqpair (Coppi 1999) are used for fitting. Using the exponentially cut-off power-law for the fits and identifying the e-folding energy with the electron temperature is dangerous, because that model does not correctly describe the shape of Comptonization continuum (see e.g. Fig. 5 in Zdziarski et al. 2003). This can result in over-estimation of T e by a factor of 3–6.

  2. Colour-magnitude diagram for the 2000 outburst of XTE J1550–564 was constructed by Russell et al. (2011), who also related the observed colours to the intrinsic spectral indices and claimed very soft spectrum of the flare. Unfortunately, all their formulae are wrong for various reasons and the actual intrinsic spectra are much harder. Furthermore, the exponential fits to the OIR light curves to evaluate the flare spectrum were also flawed, as their fits overestimate the disc contribution in the V and I filters just before the flare (see Fig. 2 in Russell et al. 2010) resulting in over-subtraction of the flux in those filters and in a much too soft spectrum of the flare (compare our α∼+0.7 at the start of the flare with their α∼−1.6).

  3. For the time lag production, this model is, however, mathematically identical to the flare evolution model.

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Acknowledgements

The work was partially supported by the Academy of Finland grant 268740 (JP) and the Finnish Doctoral Program in Astronomy and Space Physics (AV). We thank Tomaso Belloni, Andrzej Zdziarski, and Feng Yuan for valuable comments and David Russell for the data on XTE J1550–564.

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Poutanen, J., Veledina, A. Modelling Spectral and Timing Properties of Accreting Black Holes: The Hybrid Hot Flow Paradigm. Space Sci Rev 183, 61–85 (2014). https://doi.org/10.1007/s11214-013-0033-3

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  • DOI: https://doi.org/10.1007/s11214-013-0033-3

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