X-Ray Properties of Black-Hole Binaries

By Ronald A. Remillard, J. E. McClintock. 2006

1,908 citations recorded by the source corpus.

AbstractWe review the properties and behavior of 20 X-ray binaries that contain a dynamically-confirmed black hole, 17 of which are transient systems. During the past decade, many of these transien...

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/72e39b8be5481282404c8a75c8fbb1c021624298

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Citations in the corpus

Low-frequency oscillations in black holes: a spectral-timing approach to the case of GX 339-4 (2011, background): “It is also known that, even if thediskbbmodel provides a good description of the thermal component, the derived spectral parameters should not be interpreted literally (see e.g. Merloni et al. 2000, Remillard & McClintock 2006).”
Black-hole binaries, gravitational waves, and numerical relativity (2010, background): “Since neutron stars cannot have masses ∼ 3M⊙, compact objects more massive than this must be black holes (Remillard and McClintock, 2006).”
AN IMPROVED DYNAMICAL MODEL FOR THE MICROQUASAR XTE J1550−564 (2011, methodology): “…This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. outburst was observed during 2000 April–June (Rodriguez et al. 2003), and three subsequent, brief mini-outbursts were observed in 2001, 2002, and 2003 (Remillard & McClintock 2006).”
THE BLACK HOLE MASS DISTRIBUTION IN THE GALAXY (2010, background): “In Tables 1 and 2, we present basic data for all 23 confirmed black hole X-ray binaries (Remillard & McClintock 2006).”
Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes (2012, background): “Transient BHBs approach near-Eddington accretion rates near the peak of their outbursts (McClintock & Remillard 2006; Remillard & McClintock 2006; Done, Gierliński & Kubota 2007), while some exceptional BHBs spend extended periods of time with L LEdd (e.g. SS433, Margon et al. 1979; Margon 1984;…”
A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192 (2008, background): “Certainly, some binary systems consisting of a black hole and a low-mass main sequence star are observed as x-ray binaries (Remillard & McClintock 2006) with periods of ∼ 1 month.”
The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets (2007, background): “For example, could the jet outbursts sometimes seen in Galactic black hole binaries when they cross the “jet line” (Remillard & McClintock 2006) be due to rapid field annihilation and loop expulsion of the sort observed in the multiple dipolar loop simulation?”
Orbital resonances in discs around braneworld Kerr black holes (2008, background): “In fact, the black hole parameter estimates come from a varie ty of astrophysical observations [41,42,51, 60,61,50].”
Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets (2013, methodology): “Disks in the thermal state probably do not have such dissipation since their spectra show very little hard “coronal” emission (Remillard & McClintock 2006).”
Simultaneous X-ray/optical/UV snapshots of active galactic nuclei from XMM–Newton: spectral energy distributions for the reverberation mapped sample (2008, background): “…ratios seen in Galactic black holes (GBH) are often known to be correlated with particular types of accretion states: the low-flux, hard states generally exhibit low values of λEdd whereas high-flux, softer states are typically accompanied by higher values of λEdd (Remillard & McClintock 2006).”
A global spectral study of black hole X-ray binaries (2009, background): “As described in detail in Fender et al. (2004) but see also Nowak (1995); Done & Gierliński (2003); Homan & Belloni (2005); Remillard & McClintock (2006); Done et al. (2007); Belloni (2009), the outburst starts in the “low-hard” state.”
The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images (2009, methodology): “Therefore, the main targets of RXTEASM were the Galactic X-ray sources of which monitoring was suitable for performing detailed observations of these targets with an RXTE prime instrument, a large-area proportional counter array (Remillard and McClintock 2006).”
THE MASS OF THE BLACK HOLE IN CYGNUS X-1 (2011, methodology): “We processed and analyzed 2343 exposure intervals (1996 January to 2011 February; mean exposure 2.2 ks) with the Proportional Counter Array (PCA) instrument and we then computed normalized light curves in four energy bands (2–18 keV) in the manner described by Remillard & McClintock (2006).”
Evaluating Spectral Models and the X-Ray States of Neutron Star X-Ray Transients (2007, methodology): “The rms versus hard-color relations from Figure 11 can be compared with similar plots for BHs in Remillard & McClintock (2006) (panels g in their Figures 4–9).”
Influence of Cosmic Repulsion and Magnetic Fields on Accretion Disks Rotating around Kerr Black Holes (2020, methodology): “The “magnetically induced” modifications of the radial profiles of the orbital and epicyclic frequencies of the charged particle motion enable more efficient application of the magnetically modified geodesic models of the the twin HF QPOs observed in some microquasars [102] or active galactic nuclei”
Rapid optical and X-ray timing observations of GX 339-4: multi-component optical variability in the low/hard state (2010, background): “X-ray timing studies can thus provide key information for our understanding of volatile c© 2010 RAS XRB environments, and X-ray timing is now a mature field in this respect (e.g. Hasinger & van der Klis 1989; van der Klis 1995; Remillard & McClintock 2006).”
Observational evidence for intermediate-mass black holes (2017, background): “…of BHs came from X-ray and optical observations in the 1970s and 1980s of X-ray binaries (XRBs; e.g., Cygnus X-1, LMC-X3; see reviews by Casares 2006; Remillard & McClintock 2006) whose com- pact object had a mass above 3 M (i.e. too massive for a neutron star or a white dwarf; Bombaci 1996).”