Relativistic Outflows from X-ray Binaries (‘Microquasars’)

Fender, R. P.

doi:10.1007/3-540-46025-x_6

Cited by 23 publications

(26 citation statements)

References 75 publications

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“…If the two electron populations are not physically related, a likely origin of the nonthermal electrons is a relativistic jet escaping the system. In recent years, relativistic jets have revealed to be a quite common property of LMXBs, providing a link between these systems and AGNs (for a review see, e.g., Fender 2002). In this thermal plus non-thermal scenario, the Comptonized spectrum is produced by a thermal corona (likely located above the inner disk close to the boundary layer) plus a relativistic nonthermal electron jet, with the soft seed photons mainly coming from the inner disk.…”

Section: Discussionmentioning

confidence: 99%

The transient hard X-ray tail of GX 17+2: New BeppoSAX results

Farinelli¹,

Frontera

Zdziarski

et al. 2005

A&A

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Abstract. We report on results of two BeppoSAX observations of the Z source GX 17+2. In both cases the source is in the horizontal branch of the colour-intensity diagram. The persistent continuum can be fit by two-component models consisting of a blackbody plus a Comptonization spectrum. With one of these models, two solutions for the blackbody temperature of both the observed and seed photons for Comptonization are equally accepted by the data. In the first observation, when the source is on the left part of the horizontal branch, we observe a hard tail extending up to 120 keV, while in the second observation, when the source moves towards right in the same branch, the tail is no longer detected. The hard ( > ∼ 30 keV) X-ray emission can be modeled either by a simple power-law with photon index Γ ∼ 2.8, or assuming Comptonization of ∼1 keV soft photons off a hybrid thermal plus non-thermal electron plasma. The spectral index of the non-thermal injected electrons is p ∼ 1.7. The observation of hard X-ray emission only in the left part of the horizontal branch could be indicative of the presence of a threshold in the accretion rate above which the hard tail disappears. An emission line at 6.7 keV with equivalent width ∼ 30 eV is also found in both observations. We discuss these results and their physical implications.

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Section: Discussionmentioning

confidence: 99%

The transient hard X-ray tail of GX 17+2: New BeppoSAX results

Farinelli¹,

Frontera

Zdziarski

et al. 2005

A&A

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“…In general in atoll and Z sources radio emission, ascribed to the presence of a relativistic jet (Fender 2002), tends to increase towards lower S a . If this more intense jet is associated with the extra hard flux, this could cause a second branch in the CD, while the source is still in the upper banana state.…”

Section: A Jet Scenariomentioning

confidence: 91%

Peculiar spectral and power spectral behaviour of the LMXB GX 13+1

Schnerr

Reerink

Klis

et al. 2003

A&A

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Abstract. We present results of an analysis of all 480 ks of Rossi X-ray Timing Explorer Proportional Counter Array data obtained from 17 May 1998 to 11 October 1998 on the luminous low mass X-ray binary GX 13+1. We analysed the spectral properties in colour-colour diagrams (CDs) and hardness-intensity diagrams (HIDs) and fitted the power spectra with a multiLorentzian model. GX 13+1 traces out a curved track in the CDs on a time scale of hours, which is very reminiscent of a standard atoll track containing an island, and lower and upper banana branch. However, both count rate and power spectral properties vary along this track in a very unusual way, not seen in any other atoll or Z source. The count rate, which varied by a factor of ∼1.6, along a given track first decreases and then increases, causing the motion through the HIDs to be in the opposite sense to that in the CD, contrary to all other Z and atoll sources. Along a CD track, the very low frequency noise uniquely decreases in amplitude from ∼5 to ∼2% (rms). The high frequency noise amplitude decreases from ∼4% to less than 1% and its characteristic frequency decreases from ∼10 to ∼5 Hz. The 57-69 Hz quasi-periodic oscillation (QPO) found earlier is also detected, and no kHz QPOs are found. In addition the entire track shows secular motion on a time scale of about a week. The average count rate as well as the amplitude of the very low frequency noise correlate with this secular motion. We discuss a possible explanation for the peculiar properties of GX 13+1 in terms of an unusual orientation or strength of a relativistic jet.

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“…The hard state energy spectrum can physically be modelled by thermal Comptonization of cool seed photons in a hot electron plasma (Thorne & Price 1975;Shapiro et al 1976;Sunyaev & Trümper 1979;Dove et al 1998). At higher luminosities, BHs are seen in the "soft state" with a thermal X-ray spectrum with a characteristic temperature of at most a few keV, X-ray variability of only a few percent rms, and no observed radio emission (Fender 2002). The thermal X-ray spectrum in the soft state is generally associated with a geometrically thin, optically thick accretion disk (Novikov & Thorne 1973;Shakura & Sunyaev 1973;Gierliński et al 1998).…”

Section: Introductionmentioning

confidence: 99%

Long term variability of Cyg X-1

Gleissner

Wilms

Pottschmidt

et al. 2004

A&A

117

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Abstract. We study the long term evolution of the relationship between the root mean square (rms) variability and flux (the "rms-flux relation") for the black hole Cygnus X-1 as monitored from 1996 to 2003 with the Rossi X-ray Timing Explorer (RXTE). We confirm earlier results by Uttley & McHardy (2001) of a linear relationship between rms and flux in the hard state on time scales >5 s reflecting in its slope the fractional rms variability. We demonstrate the perpetuation of the linear rms-flux relation in the soft and the intermediate state. The existence of a non-zero intercept in the linear rms-flux relation argues for two lightcurve components, for example, one variable and one non-variable component, or a possible constant rms component. The relationship between these two hypothesized components can be described by a fundamental dependence of slope and intercept at time scales < ∼ 10 ksec with long term averages of the flux.

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Relativistic Outflows from X-ray Binaries (‘Microquasars’)

Cited by 23 publications

References 75 publications

The transient hard X-ray tail of GX 17+2: New BeppoSAX results

The transient hard X-ray tail of GX 17+2: New BeppoSAX results

Peculiar spectral and power spectral behaviour of the LMXB GX 13+1

Long term variability of Cyg X-1

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