Discovery of X‐Ray Jets in the Microquasar H1743−322

Corbel, S.; Kaaret, Philip; Fender, R. P.; Tzioumis, A. K.; Tomsick, John A.; Orosz, Jerome A.

doi:10.1086/432499

Cited by 203 publications

(279 citation statements)

References 28 publications

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“…A steady, compact, partially selfabsorbed jet (first imaged in Cyg X-1 by Stirling et al 2001) is present in this part of the "q"-shaped curve (region B in Fig. 1) and its radio luminosity L R also increases in correlation with the X-ray luminosity L X as L R ∝ L 0.71±0.1 X (Corbel et al 2000) or more accurately as L R ∝ L 0.6 X M 0.8 , where M is the mass of the black hole (Merloni et al 2003;Falcke et al 2004). The jet is mildly relativistic with a bulk Lorentz factor γ < 2 (Fender et al 2004a).…”

Section: Jets In Black-hole X-ray Binariesmentioning

confidence: 90%

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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Section: Jets In Black-hole X-ray Binariesmentioning

confidence: 90%

Formation and destruction of jets in X-ray binaries

Kylafis

Contopoulos

Kazanas

et al. 2012

A&A

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“…This connection gave rise to the "fundamental plane" of black hole activity. It has been found that indeed there is a close connection between the radio and X-ray luminosity of Galactic and super massive black holes of the form L radio ∝ L 0.7 X (Corbel et al 2000(Corbel et al , 2003, linking the jet activity to the total output of the central engine. Later on, a connection of these two parameters with the black hole mass itself was found, establishing the fundamental plane of AGN and Galactic black hole activity in the form of L radio ∝ L 0.6 X M 0.8 BH (e.g.…”

Section: A Fundamental Plane Of Agn Activitymentioning

confidence: 99%

The second INTEGRAL AGN catalogue

Beckmann

Soldi

Ricci

et al. 2009

A&A

167

204

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Aims. The INTEGRAL mission provides a large data set for studying the hard X-ray properties of AGN and allows testing of the unified scheme for AGN.Methods. We present analysis of INTEGRAL IBIS/ISGRI, JEM-X, and OMC data for 199 AGN supposedly detected by INTEGRAL above 20 keV. Results. The data analysed here allow significant spectral extraction on 148 objects and an optical variability study of 57 AGN. The slopes of the hard X-ray spectra of Seyfert 1 and Seyfert 2 galaxies are found to be consistent within the uncertainties, whereas higher cut-off energies and lower luminosities we measured for the more absorbed/type 2 AGN. The intermediate Seyfert 1.5 objects exhibit hard X-ray spectra consistent with those of Seyfert 1. When applying a Compton reflection model, the underlying continua appear the same in Seyfert 1 and 2 with Γ 2, and the reflection strength is about R 1, when assuming different inclination angles. A significant correlation is found between the hard X-ray and optical luminosity and the mass of the central black hole in the sense that the more luminous objects appear to be more massive. There is also a general trend toward the absorbed sources and type 2 AGN having lower Eddington ratios. The black hole mass appears to form a fundamental plane together with the optical and X-ray luminosity of the form L V ∝ L 0.6 X M 0.2 BH , similar to what is found between L R , L X , and M BH . Conclusions. The transition from the type 1 to type 2 AGN appears to be smooth. The type 2 AGN are less luminous and have less accreting super massive black holes. The unified model for Seyfert galaxies seems to hold, showing in hard X-rays that the central engine is the same in Seyfert 1 and 2, but seen under different inclination angles and absorption. The fundamental plane links the accretion mechanism with the bulge of the host galaxy and with the mass of the central engine in the same way in all types of Seyfert galaxies.

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“…These have resemblance with several other typical Galactic black hole candidates (e.g., GRO J1655-40, XTE J1550-564, GX 339-4 etc.). Another important discovery of large-scale relativistic X-ray and radio jets associated with the 2003 outburst (Rupen et al, 2004;Corbel et al, 2005) put the source in the category of 'micro-quasar'. This was also reconfirmed by McClintock et al (2009), from their comparative study on the timing and the spectral properties of this source with XTE J1550-564.…”

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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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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Discovery of X‐Ray Jets in the Microquasar H1743−322

Abstract: We report on the formation and evolution of two large-scale, synchrotron-

Cited by 203 publications

References 28 publications

Formation and destruction of jets in X-ray binaries

Formation and destruction of jets in X-ray binaries

The second INTEGRAL AGN catalogue

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

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