Relativistic motion in a nearby bright X-ray source

Tingay, S. J.; Jauncey, D. L.; Preston, R. A.; Reynolds, John E.; Meier, David L.; Murphy, D. W.; Tzioumis, A. K.; McKay, D. J.; Kesteven, Michael; Lovell, J. E. J.; Campbell-Wilson, D.; Elllngsen, S. P.; Gough, R. G.; Hunstead, R. W.; Jonos, D. L.; McCulloch, P. M.; Migenes, V.; Quick, J.; Sinclair, M. W.; Smits, Derck P.

doi:10.1038/374141a0

Cited by 284 publications

(211 citation statements)

References 6 publications

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“…Thus, high sensitivity, high-angular-resolution radio observations with good snapshot (u, v)-coverage are required to enable high time resolution 'movies' of these relativistic outflows and avoid the problems that arise from rapid evolution of the jet morphology and brightness within a single observation Tingay et al 1995;Mioduszewski et al 2001). Such observations are crucial in order to tie jetejection events to X-ray timing and spectral changes in the accretion flow.…”

Section: Jet Formation and Evolutionmentioning

confidence: 99%

Science at Very High Angular Resolution with the Square Kilometre Array

Godfrey

Bignall

Tingay

et al. 2012

Publ. – Astron. Soc. Aust

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Preliminary specifications for the Square Kilometre Array (SKA) call for 25% of the total collecting area of the dish array to be located at distances greater than 180 km from the core, with a maximum baseline of at least 3000 km. The array will provide angular resolution y t 40-2 mas at 0.5-10 GHz with image sensitivity reaching t50 nJy beam À1 in an 8-hour integration with 500-MHz bandwidth. Given these specifications, the high-angular-resolution component of the SKA will be capable of detecting brightness temperatures t200 K with milliarcsecond-scale angular resolution. The aim of this article is to bring together in one place a discussion of the broad range of new and important high-angular-resolution science that will be enabled by the SKA, and in doing so, address the merits of long baselines as part of the SKA. We highlight the fact that high angular resolution requiring baselines greater than 1000 km provides a rich science case with projects from many areas of astrophysics, including important contributions to key SKA science.

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Section: Jet Formation and Evolutionmentioning

confidence: 99%

Science at Very High Angular Resolution with the Square Kilometre Array

Godfrey

Bignall

Tingay

et al. 2012

Publ. – Astron. Soc. Aust

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“…Prior to the launch of RXTE, only two microquasars were known among the population of BHs: GRS 1915+105 (see Fig. 2 from [8]) and GRO J1655−40 [9,10]. Since then, the number of BHs displaying apparent superluminal motion has greatly increased.…”

Section: Transient Jet Ejection Eventsmentioning

confidence: 99%

Relativistic Jets in the RXTE Era

Corbel

2004

AIP Conference Proceedings

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Abstract.Since the launch of the Rossi X-ray Timing Explorer in 1995 our understanding of jetted outflows has significantly improved. Indeed, relativistic jets are now believed to be a fairly ubiquitous property of accreting compact objects, that are intimately coupled with the accretion history. In this review, we summarize the observational connections in X-ray binaries between accretion flows and relativistic outflows (especially the relation with the X-ray states). We emphasize those aspects that have significantly benefited from the RXTE experiment, including the role that jets could play at high energies. We also review recent observations of large scale relativistic jets that could point to their long term effects on the interstellar medium. BLACK HOLE CANDIDATES AND X-RAY STATESBlack hole candidates (hereafter BH, even if its mass function has not been measured) are known to exhibit several X-ray spectral states, distinguished by the presence or absence of a soft black-body component at ∼ 1 keV (arising from the accretion disk) and the luminosity and spectral slope of emission at harder energies (whose nature is still the subject of an active debate). Systems in the low-hard state (LHS) have power-law X-ray spectra with a photon index in the range 1.4-1.9, an exponential cutoff (but not always) around 100 keV, and no (or only weak) evidence of a soft thermal component. In the LHS, the power density spectrum (PDS) is characterized by a strong band-limited noise power continuum. At higher soft X-ray flux 1 , these systems are usually found in the thermal-dominant (TD) or high-soft (HS) state. In that case, the X-ray spectrum is dominated (up to ∼ 90%) by the soft-thermal component, with an additional weak and steep power-law component (with no apparent cut-off) at higher energy. very weak residual X-ray emission that displays many similarities with the LHS [e.g. 4,5]. This implies that the QS could simply be a low luminosity version of the LHS. With the detailed coverage by RXTE of spectral properties of BHs during recent outbursts, the different X-ray states can be well illustrated using a HardnessIntensity diagram (see Fig. 1 from [6]). In this case, the VHS and IS are defined as various tracks between the vertical tracks (of constant hardness) of the HS and LHS [2,6]. For further details on the spectral states of BH, see [3]. In the sections that follow, we discuss the general properties of BHs in the various X-ray states, some of which they have in common with neutron star (NS) systems, and focus on relativistic jets in the light of recent developments based on multi-wavelength observations (including RXTE). For a detailed reviews of jets in X-ray binaries, see [7].

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“…The radio emission of such episodic jet originates from an optically thin synchrotron emission component and the Lorentz factor of the ejected plasmoids is usually much larger than that of the continuous jet, and sometimes these episodic jets appear superluminal (e.g. GRS 1915+105, Mirabel & Rodríguez 1994Fender et al 1999;GRO J1655-40, Hjellmin & Rupen 1995Tingay et al 1995;XTE J1748-288, Brocksopp et al 2007). The emission from the episodic jet is probably more polarized than the continuous jet .…”

Section: Introductionmentioning

confidence: 99%

“…At this time, the continuous jet has already faded. The radio flares are associated c 0000 RAS with plasmoids ejections, and sometimes can be resolved by radio observations, such as the jets seen in GRS 1915+105 (Mirabel & Rodríguez 1994;Fender et al 1999), GRO J1655-40 (Hjellmin & Rupen 1995Tingay et al 1995), XTE J1550-564 (Corbel et al 2002), H 1743-322 (Miller-Jones et al 2012 and XTE J1752-223 (Yang et al 2010(Yang et al , 2011. The radio emission of such episodic jet originates from an optically thin synchrotron emission component and the Lorentz factor of the ejected plasmoids is usually much larger than that of the continuous jet, and sometimes these episodic jets appear superluminal (e.g.…”

Section: Introductionmentioning

confidence: 99%

Discovery of the correlation between peak episodic jet power and X-ray peak luminosity of the soft state in black hole transients

Zhang¹,

Yu²

2015

Monthly Notices of the Royal Astronomical Society

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Episodic jets are usually observed in the intermediate state of black hole transients during their X-ray outbursts. Here we report the discovery of a strong positive correlation between the peak radio power of the episodic jet P jet and the corresponding peak X-ray luminosity L x of the soft state (in Eddington units) in a complete sample of the outbursts of black hole transients observed during the RXTE era of which data are available, which follows the relation log P jet = (2.2 ± 0.3) + (1.6 ± 0.2) × log L x . The transient ultra-luminous X-ray source in M31 and HLX-1 in EXO 243-49 fall on the relation if they contain stellar mass black hole and either stellar mass black hole or intermediate mass black hole, respectively. Besides, a significant correlation between the peak power of the episodic jet and the rate-of-increase of the X-ray luminosity dL x /dt during the rising phase of those outbursts is also found, following log P jet = (2.0 ± 0.4) + (0.7 ± 0.2) × log dL x /dt. In GX 339−4 and H 1743−322 in which data for two outbursts are available, measurements of the peak radio power of the episodic jet and the X-ray peak luminosity (and its rate-of-change) shows similar positive correlations between outbursts, which demonstrate the dominant role of accretion over black hole spin in generating episodic jet power. On the other hand, no significant difference is seen among the systems with different measured black hole spin in current sample. This implies that the power of the episodic jet is strongly affected by non-stationary accretion instead of black hole spin characterized primarily by the rate-of-change of the mass accretion rate.

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Relativistic motion in a nearby bright X-ray source

Cited by 284 publications

References 6 publications

Science at Very High Angular Resolution with the Square Kilometre Array

Science at Very High Angular Resolution with the Square Kilometre Array

Relativistic Jets in the RXTE Era

Discovery of the correlation between peak episodic jet power and X-ray peak luminosity of the soft state in black hole transients

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