Radio emission from conical jets associated with X-ray binaries

Hjellming, R. M.; Johnston, K. J.

doi:10.1086/166318

Cited by 235 publications

(260 citation statements)

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“…We assume a simple synchrotron-emitting bubble model, in which a spherical cloud is expanding adiabatically and isotropically. Using the wellknown formula for the temporal process of observed flux (van der Laan 1966;Hjellming & Johnston 1988;Ishwara et al 2002), a power-law index of electron energy distribution [N (E ) dE / E À dE ] is given from single-frequency observations. The index is given as…”

Section: Discussionmentioning

confidence: 99%

High and Low Galactic Latitude Radio Transients in the Nasu 1.4 GHz Wide-Field Survey

et al. 2007

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We report the detection of two radio transients in the Nasu 1.4 GHz wide-field survey. In the survey, we use four pairs of the two-element interferometer aligned east-west to monitor the wide-field sky and simultaneously survey the region at þ32 < < þ42 in drift scanning. In 27 days of continuous observation at a declination between +41 and +42 , we have detected two radio transients of 1 Jy intensity. Since they appeared on only a single day during the 27 days, we consider these detections to be 1 Jy class bursts that brightened and faded within 2 days and have constant emission smaller than 200 mJy, the detection limit of the 27 days of integrated data. While one transient was in low Galactic latitudes, the other transient was detected in high Galactic latitudes and has counterparts only in -ray databases. Therefore, the high Galactic latitude transient might be one of the active galactic nuclei that are normally very faint in X-ray and quiet in radio wavelengths.

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Section: Discussionmentioning

confidence: 99%

High and Low Galactic Latitude Radio Transients in the Nasu 1.4 GHz Wide-Field Survey

et al. 2007

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“…At the same time, the jet pattern speed v n v j (1 + (v j /v φ ) 2 ) −0.5 , where v φ is the azimuthal velocity of the jet due to the precession and nutation, may be large enough to excite the shock waves on the surface, which spread inside the jet and cause strong turbulence around the clouds in the jet and, as a result, strengthen the magnetic field and very effectively accelerate relativistic particles, as was shown for supernova remnants by Inoue et al, (2012). Therefore, in contrast to the model of Hjellming & Johnston, (1988), in our model the synchrotron emission occurs not on the surface of a homogeneous jet, but in the vicinity of the dense clouds, and the jet is not adiabatic, but is heating to temperatures T > ∼ 10 7 K downward of the jet (Migliari et al, 2002).…”

Section: Dynamics Of Ss 433 Jetsmentioning

confidence: 93%

Simulation of kinematics of SS 433 radio jets that interact with the ambient medium

Panferov

2014

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Context. The mildly relativistic jets of SS 433 are believed to inflate the surrounding supernova remnant W 50, possibly depositing more than 99% of their kinetic energy in the remnant expansion. Where and how this transformation of the energy occurs is as yet unknown. We can learn from this that the jets decelerate and that this deceleration is non-dissipative. Aims. We uncover the deviation of the arcsecond-scale precessing radio jets of SS 433 from the ballistic locus described by the kinematic model as a signature of the dynamics issuing from the interaction of the jets with the ambient medium. Methods. To do this, we simulated the kinematics of these jets, taking into account the ram pressure on the jets, which we estimated from the profile of brightness of synchrotron radiation along the radio jets, assuming pressure balance in the jets. Results. We found that to fit an observable locus in all scales the radio jets need to be decelerated and twisted in addition to the precession torsion, mostly within the first one-fifth of the precession period, and subsequently they extend in a way that imitates ballistic jets. This jet kinematics implies a smaller distance to SS 433 than the currently accepted 5.5 kpc. The physical parameters of the jet model, which links jets dynamics with radiation, are physically reliable and characteristic for the SS 433 jets. The model proposes that beyond the radio-brightening zone, the jet clouds expand because they are in pressure balance with the intercloud medium, and heat up with distance according to the law T = 2 × 10 4 (r/10 15 cm) 1.5 K. Conclusions. This model naturally explains and agrees with, the observed properties of the radio jets: a) the shock-pressed morphology; b) the brightness profile; c) the ∼10% deflections of the jet kinematics from the standard kinematic model -a magnitude of the jet speed decrement in our simulation; d) the precession-phase deviations from the standard kinematic model predictions; e) the dichotomy of the distances to the object, 4.8 kpc vs. 5.5 kpc, which are determined on the basis of the jet kinematics on scales of sub-arcsecond and several arcseconds, respectively; and f) the reheating on arcsecond scales.

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“…For example, for the inflowing component, there can be a contribution from a RIAF (e.g., Remillard & McClintock 2006) and/or an efficient thin disk (e.g., Miller et al 2006;Wilkinson & Uttley 2009;Reis, Fabian & Miller 2010;Reynolds & Miller 2013), and the relative balance between the two types of flows might not be universal for every source. Regardless, it is well-established that hard state BHXBs are associated with compact radio emission, which is interpreted as optically thick synchrotron radiation from the partially self-absorbed flat spectral component of a compact relativistic jet (Blandford & Königl 1979;Hjellming & Johnston 1988;Fender 2001). The compact jet typically remains unresolved in the radio, except for in a handful of cases with high (very long baseline interferometric) spatial resolution imaging (e.g., GRS 1915+105; Cyg X-1; Dhawan, Mirabel & Rodríguez 2000;Stirling et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Constraints on relativistic jets in quiescent black hole X-ray binaries from broad-band spectral modelling

Plotkin

Gallo

Markoff

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The nature of black hole jets at the lowest detectable luminosities remains an open question, largely due to a dearth of observational constraints. Here, we present a new, nearly-simultaneous broadband spectrum of the black hole X-ray binary (BHXB) XTE J1118+480 at an extremely low Eddington ratio (L X ∼ 10 −8.5 L Edd ). Our new spectral energy distribution (SED) includes the radio, near-infrared, optical, ultraviolet, and X-ray wavebands. XTE J1118+480 is now the second BHXB at such a low Eddington ratio with a well-sampled SED, thereby providing new constraints on highly sub-Eddington accretion flows and jets, and opening the door to begin comparison studies between systems. We apply a multi-zone jet model to the new broadband SED, and we compare our results to previous fits to the same source using the same model at 4-5 decades higher luminosity. We find that after a BHXB transitions to the so-called quiescent spectral state, the jet base becomes more compact (by up to an order of magnitude) and slightly cooler (by at least a factor of two). Our preferred model fit indicates that jet particle acceleration is much weaker after the transition into quiescence. That is, accelerated non-thermal particles no longer reach high enough Lorentz factors to contribute significant amounts of synchrotron X-ray emission. Instead, the X-ray waveband is dominated by synchrotron self-Compton emission from a population of mildly relativistic electrons with a quasi-thermal velocity distribution that are associated with the jet base. The corresponding (thermal) synchrotron component from the jet base emits primarily in the infrared through ultraviolet wavebands. Our results on XTE J1118+480 are consistent with broadband modeling for A0620-00 (the only other comparably low Eddington ratio BHXB with a well-sampled SED) and for Sgr A* (the quiescent supermassive black hole at the Galactic center). The above could therefore represent a canonical baseline geometry for accreting black holes in quiescence. We conclude with suggestions for future studies to further investigate the above scenario.

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Radio emission from conical jets associated with X-ray binaries

Cited by 235 publications

References 0 publications

High and Low Galactic Latitude Radio Transients in the Nasu 1.4 GHz Wide-Field Survey

High and Low Galactic Latitude Radio Transients in the Nasu 1.4 GHz Wide-Field Survey

Simulation of kinematics of SS 433 radio jets that interact with the ambient medium

Constraints on relativistic jets in quiescent black hole X-ray binaries from broad-band spectral modelling

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