Jet-dominated advective systems: radio and X-ray luminosity dependence on the accretion rate

Körding, Elmar; Fender, R. P.; Migliari, S.

doi:10.1111/j.1365-2966.2006.10383.x

Cited by 159 publications

(211 citation statements)

References 62 publications

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“…They proposed that the jet kinetic power of where r is the radio spectral index over the partially self-absorbed regime, and the parameter W 37:8 carries the (quite large) uncertainty on the radio galaxy calibration. The normalization value by Heinz & Grimm is roughly in agreement with that estimated by Körding et al (2006); here, for flat spectrum radio sources, the jet power (at the hard to soft state transition) is expressed as L j;tot P 3:6 ; 10 37 ( f =0:…”

Section: Origin Of the Mid-ir Excess: Implications For The Jet Powersupporting

confidence: 84%

The Spectral Energy Distribution of Quiescent Black Hole X‐Ray Binaries: New Constraints fromSpitzer

Gallo¹,

Migliari²,

Markoff³

et al. 2007

ApJ

110

174

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Among the various issues that remain open in the field of accretion onto black hole X-ray binaries (BHBs) is the question of how gas accretes at very low Eddington ratios, in the so-called quiescent regime. While there is general agreement that X-rays are produced by a population of high-energy electrons near the BH, there is controversy concerning the modeling of the contributions of inflowing versus outflowing particles and their relative energy budget. Recent Spitzer observations of three quiescent BHBs have shown evidence for excess emission with respect to the Rayleigh-Jeans tail of the companion star between 8Y24 m. We suggest that synchrotron emission from a partially self-absorbed outflow might be responsible for the observed mid-IR excess, in place of, or in addition to, thermal emission from circumbinary material. If so, then the jet synchrotron luminosity, integrated from radio to near-IR frequencies, exceeds the measured 2Y10 keV luminosity by a factor of a few in these systems. In turn, the mechanical power stored in the jet exceeds the bolometric X-ray luminosity by at least 4 orders of magnitude. We compile the broadband spectral energy distribution (SED) of A0620À00, the lowest Eddington-ratio stellar mass BH with a known radio counterpart, by means of simultaneous radio, optical, and X-ray observations, and the archival Spitzer data. We are able to fit the SED of A0620À00 with a maximally jet-dominated model, in which the radio through the soft X-rays are dominated by synchrotron emission, while the hard X-rays are dominated by inverse Compton at the jet base. The fitted parameters land in a range of values reminiscent of the Galactic center supermassive black hole Sgr A Ã . Most notably, the inferred ratio of the jet acceleration rate to local cooling rates is 2 orders of magnitude weaker than higher luminosity, hard-state sources.

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Section: Origin Of the Mid-ir Excess: Implications For The Jet Powersupporting

confidence: 84%

The Spectral Energy Distribution of Quiescent Black Hole X‐Ray Binaries: New Constraints fromSpitzer

Gallo¹,

Migliari²,

Markoff³

et al. 2007

ApJ

110

174

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“…They are named atoll and Z sources (Hasinger & van der Klis 1989) because of the shape that they trace in a color-color diagram. Both classes exhibit jets, but because their radio emission is weaker than that in black-hole XRBs, they have received less attention (for comprehensive reviews of the properties of jets from neutron-star XRBs, see Körding et al 2006). Moreover, neutron stars are more complex than black holes in that they possess a solid surface and a stellar magnetic field.…”

Section: Jets In Neutron-star X-ray Binariesmentioning

confidence: 99%

Formation and destruction of jets in X-ray binaries

Kylafis

Contopoulos

Kazanas

et al. 2012

A&A

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Context. Neutron-star and black-hole X-ray binaries (XRBs) exhibit radio jets, whose properties depend on the X-ray spectral state and history of the source. In particular, black-hole XRBs emit compact, steady radio jets when they are in the so-called hard state. These jets become eruptive as the sources move toward the soft state, disappear in the soft state, and then re-appear when the sources return to the hard state. The jets from neutron-star X-ray binaries are typically weaker radio emitters than the black-hole ones at the same X-ray luminosity and in some cases radio emission is detected in the soft state. Aims. Significant phenomenology has been developed to describe the spectral states of neutron-star and black-hole XRBs, and there is general agreement about the type of the accretion disk around the compact object in the various spectral states. We investigate whether the phenomenology describing the X-ray emission on one hand and the jet appearance and disappearance on the other can be put together in a consistent physical picture. Methods. We consider the so-called Poynting-Robertson cosmic battery (PRCB), which has been shown to explain in a natural way the formation of magnetic fields in the disks of AGNs and the ejection of jets. We investigate whether the PRCB can also explain the formation, destruction, and variability of jets in XRBs. Results. We find excellent agreement between the conditions under which the PRCB is efficient (i.e., the type of the accretion disk) and the emission or destruction of the radio jet. Conclusions. The disk-jet connection in XRBs can be explained in a natural way using the PRCB.

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“…Kording et al 2006;Kording et al 2008;Tudose et al 2009), argues for an ejection process that is also independent of the central object. This seems to be confirmed by the lack of correlation between jet power or jet velocities and measured values of black hole spins (Fender et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Relevance of jet emitting disc physics to microquasars: application to Cygnus X-1

Petrucci

Ferreira

Henri

et al. 2010

A&A

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Context. Interpretation of the X-ray spectra of X-ray binaries during their hard states requires a hot, optically thin medium. There are several accretion disc models that account for this aspect. However, none is designed to simultaneously explain powerful jets detected during these states. Aims. A new quasi-Keplerian hot accretion disc solution, a jet emitting disc (JED hereafter), which is part of a global disc-jet MHD structure producing stationary super-alfvénic ejection, is investigated here. Its radiative and energetic properties are then compared to the observational constraints found in Cygnus X-1. Methods. We solve the disc energy equation by balancing the local heating term with advection and cooling by synchrotron, bremsstrahlung, and Comptonization processes. The heating term, disc density, accretion velocity, and magnetic field amplitude were taken from published self-similar models of accretion-ejection structures. Both optically thin and thick regimes are considered in a one-temperature, gas-supported disc. Results. Three branches of solutions are found to be possible at a given radius, but we only investigate the hot, optically thin and geometrically slim solutions. These solutions give simultaneously and consistently the radiative and energetics properties of the discjet system. They are able to reproduce the global accretion-ejection properties of Cygnus X-1 very well, namely its X-ray spectral emission, jet power, and jet velocity. About half of the released accretion power is used to produce two mildly relativistic (v/c 0.5) jets, and for a luminosity of about 1% of the Eddington luminosity, the JED temperature and optical depth are close to what is observed in the hard state of Cygnus X-1. Conclusions. The accretion and ejection properties of JEDs agree with the observations of the prototypical black hole binary Cygnus X-1. The JED solutions are likely to be relevant to the whole class of microquasars.

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Jet-dominated advective systems: radio and X-ray luminosity dependence on the accretion rate

Cited by 159 publications

References 62 publications

The Spectral Energy Distribution of Quiescent Black Hole X‐Ray Binaries: New Constraints fromSpitzer

The Spectral Energy Distribution of Quiescent Black Hole X‐Ray Binaries: New Constraints fromSpitzer

Formation and destruction of jets in X-ray binaries

Relevance of jet emitting disc physics to microquasars: application to Cygnus X-1

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