GRS 1915+105 and the Disc-Jet Coupling in Accreting Black Hole Systems

By Robert P. Fender, T. Belloni. 2004

329 citations recorded by the source corpus.

▪ Abstract GRS 1915+105—the first stellar-scale, highly relativistic jet source identified—is a key system for our understanding of the disc-jet coupling in accreting black hole systems. Comprehending the coupling between inflow and outflow in this source not only is important for X-ray binary systems but has a broader relevance for studies of active galactic nuclei and gamma-ray bursts. In this paper, we present a detailed review of the observational properties of the system, as established in the decade since its discovery. We attempt to place it in context by a detailed comparison with other sources, and construct a simple model for the disc-jet coupling, which may be more widely applicable to accreting black hole systems.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fc01b0f3b6a4dcad6f5fe138959ca15f94037e3e

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Citations in the corpus

Hot Accretion Flows Around Black Holes (2014, background): “Other differences have been noted in the polarization, spectrum, and power (Fender & Belloni 2004).”
Using the Fundamental Plane of black hole activity to distinguish X-ray processes from weakly accreting black holes (2011, background): “…state transitions marked by different contributions of hard non-thermal X-ray emission (from a jet/corona) to the total observed X-ray flux, where softer X-rays are emitted by the accretion disc (see e.g. Fender & Belloni 2004; McClintock 2004; Homan & Belloni 2005; Fender, Homan & Belloni 2009).”
Flaring Activity of Sagittarius A* at 43 and 22 GHz: Evidence for Expanding Hot Plasma (2006, methodology): “…the jet model has been successfully applied to a number of sources such as GRS 1915+105 (e.g., Mirabel et al. 1998; Fender & Pooley 1998; Fender & Belloni 2004) and Cyg X-3 where the frequency dependent of the peak flux density is in the optically thick domain due to synchrotron…”
X-Ray Properties of Black-Hole Binaries (2006, background): “Such ejections have been observed for at least eight BHBs and BHCs (Mirabel & Rodriguez 1999; Fender & Belloni 2004; McClintock & Remillard 2006 and references therein).”
Klein-Nishina effects in the spectra of non-thermal sources immersed in external radiation fields (2005, background): “However, GRS 1915+105 proves that X-ray binaries (XRBs) have the ability to produce much more powerful and relativistic jets (Fender & Belloni 2004) than in the sources just mentioned.”
General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems (2006, background): “GRS 1915+105 has a mass accretion rate of Ṁ ∼ 7 × 10−7M⊙ yr−1 (Mirabel & Rodriguez 1994; Mirabel & Rodŕıguez 1999; Fender & Belloni 2004) with a mass of M ∼ 14M⊙ (Greiner et al. 2001), but see Kaiser et al. (2004).”
Radio sources in low-luminosity active galactic nuclei IV. Radio luminosity function, importance of jet power, and radio properties of the complete Palomar sample (2005, background): “Interestingly, compact flat spectrum radio nuclei are also detected toward the ∼10−15 M black holes in Galactic X-ray binary sources, especially during phases of highly sub-Eddington accretion (see review by Fender & Belloni 2004).”
Jets from black hole X-ray binaries: testing, refining and extending empirical models for the coupling to X-rays (2009, background): “…reader that while we do not discuss this source specifically here, the large number of events observed from the powerful jet source GRS 1915+105 (Fender & Belloni 2004) are all, to our knowledge, consistent with the patterns described in FBG04(see also Soleri, Belloni & Casella 2008 for the…”
Observational evidence for a correlation between jet power and black hole spin (2011, background): “As most clearly demonstrated for the prototype microquasar GRS 1915+105 (Fender & Belloni 2004), this stage appears to correspond to the inward-moving inner edge of the accretion disc reaching the ISCO, which results in a shock or some other violent event that launches the large-scale relativistic…”
Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets (2013, methodology): “…by using the disk X-ray luminosity as a proxy for ˙ M (e.g., Heinz & Sunyaev 2003; Merloni et al. 2003; Falcke et al. 2004; Fender et al. 2004; Fender & Belloni 2004), but one must have knowledge of the radiative eﬃciency of the disk, which is generally both low and variable in the hard…”
No evidence for black hole spin powering of jets in X-ray binaries (2010, methodology): “For both the radio and infrared data sets, we include a ‘representative’ measurement for the hard ‘plateau’ state of GRS 1915+105 (Fender & Belloni 2004).”
Testing the Kerr Black Hole Hypothesis Using X-Ray Reflection Spectroscopy (2016, background): “If the inner 8 Blum et al. (2009) estimate the Eddington-scaled accretion luminosity of the source∼0.3, but they assume the black hole mass M=14±4 Me (Greiner et al. 2001) and distance D∼12 kpc (Fender & Belloni 2004).”
Supermassive black holes in elliptical galaxies: switching from very bright to very dim (2005, background): “For individual binaries the radio emission has been observed to vary depending on the X-ray flux and on the spectral state of the source (e.g. Fender & Belloni 2004).”
A Unified Model for Black Hole X-Ray Binary Jets? (2004, methodology): “The reason for which is that the thermal disccomponent in GRS 1915+105 is considerably higher than in other systems (see Fender & Belloni 2004): using the same energy bands results in the harder C state having a softer color than the soft r B state.”
THE EXTREME SPIN OF THE BLACK HOLE IN CYGNUS X-1 (2011, background): “Three have low to moderate spins, a∗ <∼ 0.5; four have high spins,a∗ ∼ 0.7 − 0.9; and one of them, the archetypal microquasar GRS 1915+105 (Mirabel & Rodrı́guez 1994; Fender & Belloni 2004), is a near-extreme Kerr hole witha∗ > 0.98 (McClintock et al. 2006; Blum et al. 2009).”
Total and Jet Blandford-Znajek Power in the Presence of an Accretion Disk (2005, background): “For example, the black hole X-ray binary GRS 1915 05 has a jet with apparently superluminal motion withG ∼ 1.5–3 (Mirabel & Rodrı́guez 1994, 1999; Fender & Belloni 2004; Kaiser et al. 2004).”
WATCHDOG: A COMPREHENSIVE ALL-SKY DATABASE OF GALACTIC BLACK HOLE X-RAY BINARIES (2015, background): “…variability, such as QPOs ranging in frequency from 10−3 Hz to 67 Hz and patterns of dips and rapid transitions between high and low intensity in the light curve (Greiner et al. 1996; Morgan et al. 1997; Belloni et al. 2000; Klein-Wolt et al. 2002; Fender & Belloni 2004; Hannikainen et al. 2005).”
Radiative efficiency, variability and Bondi accretion on to massive black holes: the transition from radio AGN to quasars in brightest cluster galaxies (2012, background): “Gallo, Fender & Pooley 2003; Fender & Belloni 2004).”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, background): “Also, a few black hole x-ray binaries spend significant periods of time with L & LEdd (e.g., SS433, Margon et al. 1979; Margon 1984; Takeuchi et al. 2010; GRS1915+105, Fender & Belloni 2004).”
Populations of X-Ray Sources in Galaxies (2006, background): “…functions of the Galactic X-ray source populations; White, Nagase & Parmar 1995 for a review of the properties of Galactic X-ray binaries; Verbunt & van den Heuvel 1995 for a review on the formation and evolution of XRBs; Fender & Belloni 2004 on the spectral states of black-hole binaries).”