X-Ray Emission From Transient Jet Model in Black Hole Binaries

Pe’er, Asaf; Markoff, Sera

doi:10.1088/0004-637x/753/2/177

Cited by 27 publications

(29 citation statements)

References 79 publications

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“…Since it preferentially occurs at low luminosities ( ∼ < 10 −3 L Edd ), where count rates are usually too low for accurate spectral fitting, and since it seems to have a similar power law index and timing properties to the Comptonized corona (see also Casella et al 2010), this synchrotron component has probably been largely overlooked so far. As has been demonstrated, the polarization properties of the synchrotron and Comptonization X-ray power laws are expected to differ, so differentiating between these two emission mechanisms will be possible with future X-ray polarimeters (see also Pe'er & Markoff 2012). For jet synchrotron emission, X-ray FLP of a few per cent could be detected, with variability in FLP on short timescales.…”

Section: Evidence For a Jet Contribution To The X-raymentioning

confidence: 93%

The multiwavelength polarization of Cygnus X–1

Russell¹,

Shahbaz²

2014

Monthly Notices of the Royal Astronomical Society

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Polarization measurements of the microquasar Cygnus X-1 exist at γ-ray, X-ray, UV, optical and radio frequencies. The γ-ray emission has been shown to be highly linearly polarized. Here, we present new infrared polarimetric data of Cygnus X-1 taken with the 10.4-m Gran Telescopio Canarias and the 4.2-m William Herschel Telescope. We show that the broadband, radio to γ-ray flux spectrum and polarization spectrum in the hard state are largely consistent with a simple phenomenological model of a strongly polarized synchrotron jet, an unpolarized Comptonized corona and a moderately polarized interstellar dust component. In this model, the origin of the γ-ray, X-ray and some of the infrared polarization is the optically thin synchrotron power law from the inner regions of the jet. The model requires the magnetic field in this region to be highly ordered and perpendicular to the axis of the resolved radio jet. This differs to studies of some other X-ray binaries, in which the magnetic field is turbulent, variable and aligned with the jet axis. The model is able to explain the approximate polarization strength and position angle at all wavelengths including the detected X-ray (3-5 keV) polarization, except the observed position angle of the γ-ray polarization, which differs to the model by ∼ 60 • . Past numerical modelling has shown that a curved synchrotron spectrum can produce a shift in position angle by ∼ 60 • , which may account for this.

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Section: Evidence For a Jet Contribution To The X-raymentioning

confidence: 93%

The multiwavelength polarization of Cygnus X–1

Russell¹,

Shahbaz²

2014

Monthly Notices of the Royal Astronomical Society

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“…Díaz Trigo et al 2018), although their evolution with accretion flow geometry remain unclear. Additionally, while the location and behaviour of the high-energy synchrotron cooling break is not well understood (Pe'er & Markoff 2012;Shahbaz et al 2013;Gardner & Done 2013), its position and evolution will dictate the total radiative jet power (Russell et al 2014). Therefore, simply comparing the 6 GHz luminosity would disregard a large fraction of jet power during the giant outburst.…”

Section: What Do the X-ray And Radio Luminosity Trace?mentioning

confidence: 99%

A re-establishing jet during an X-ray re-brightening of the Be/X-ray binary Swift J0243.6+6124

Eijnden

Degenaar

Russell

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Transient Be/X-ray binary systems, wherein a compact object accretes from a Becompanion star, can show giant and periastron outbursts. During the decay of their giant outbursts, some Be/X-ray binaries also show X-ray re-brightenings, the origin of which is not understood. Recently, we presented the discovery of a jet from a neutron star Be/X-ray binary, observed during the giant outburst of Swift J0243.6+6124. Here, we present continued radio monitoring of its 2017/2018 giant outburst decay and a re-brightening of this source. During the former, we observe a radio flare with a steep radio spectrum, possibly caused by interactions between discrete ejecta colliding with the pre-existing jet or the surrounding medium. During the X-ray re-brightening, we observe the radio jet turning on and off within days. Surprisingly, this re-establishing jet is as bright in radio as at the peak of the super-Eddington giant outburst, despite more than two orders of magnitude lower X-ray luminosity. In addition, the jet is only observed when the X-ray luminosity exceeds approximately 2 × 10 36 (D/5kpc) 2 erg/s. We discuss how such an X-ray threshold for jet launching might be related to the presence of a magnetic centrifugal barrier at lower mass accretion rates. We also discuss the implications of our results for the launch of jets from strongly magnetized neutron stars, and explore future avenues to exploit the new possibility of coordinated X-ray/radio studies of neutron star Be/X-ray binaries.

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“…For the model discussed in Pe'er & Markoff (2012), the electrons at the jet base characteristically produce a power law with a photon index of around 1.5 and a break at higher energies. The location of the break is determined by the acceleration mechanism whose details are uncertain.…”

Section: High Energy Breaks and Jetsmentioning

confidence: 99%

“…According to Pe'er & Markoff (2012), a distinct feature of synchrotron radiation at hard X-rays would be a photon index of around 1.5 before a gradual break in the spectrum at ∼10 keV caused by rapid cooling of electrons. Characterizing properties of spectral breaks at hard X-rays therefore is important to test predictions of jet models, especially when these models incorporate detailed electron acceleration mechanisms Using HEXTE on RXTE, Miyakawa et al (2008) investigated the relation between the cut-off energy (from the fits with cut-off power-law) and several other spectral parameters from all hard state observations of GX 339−4, and found an inverse correlation between the cut-off energy and luminosity for the bright hard state observations.…”

mentioning

confidence: 99%

Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

Kalemci

Arabacı

Güver

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We characterized the broad-band X-ray spectra of Swift J1745−26 during the decay of the 2013 outburst using INTEGRAL ISGRI, JEM-X and Swift XRT. The X-ray evolution is compared to the evolution in optical and radio. We fit the Xray spectra with phenomenological and Comptonization models. We discuss possible scenarios for the physical origin of a ∼50 day flare observed both in optical and Xrays ∼170 days after the peak of the outburst. We conclude that it is a result of enhanced mass accretion in response to an earlier heating event. We characterized the evolution in the hard X-ray band and showed that for the joint ISGRI-XRT fits, the e-folding energy decreased from 350 keV to 130 keV, while the energy where the exponential cut-off starts increased from 75 keV to 112 keV as the decay progressed. We investigated the claim that high energy cut-offs disappear with the compact jet turning on during outburst decays, and showed that spectra taken with HEXTE on RXTE provide insufficient quality to characterize cut-offs during the decay for typical hard X-ray fluxes. Long INTEGRAL monitoring observations are required to understand the relation between the compact jet formation and hard X-ray behavior. We found that for the entire decay (including the flare), the X-ray spectra are consistent with thermal Comptonization, but a jet synchrotron origin cannot be ruled out.

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X-Ray Emission From Transient Jet Model in Black Hole Binaries

Cited by 27 publications

References 79 publications

The multiwavelength polarization of Cygnus X–1

The multiwavelength polarization of Cygnus X–1

A re-establishing jet during an X-ray re-brightening of the Be/X-ray binary Swift J0243.6+6124

Multiwavelength observations of the black hole transient Swift J1745−26 during the outburst decay

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