Excitation of low-frequency QPOs in black hole accretion

Giannios, Dimitrios; Spruit, H. C.

doi:10.1051/0004-6361:200400043

Cited by 27 publications

(34 citation statements)

References 46 publications

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“…Fig. 1 and Section 3) and the QPO relates with the orbital frequency (Keplerian) at R tr (Giannios & Spruit 2004), then we have R tr ∼ 1.1 × 10 4 R s (Shahbaz et al 2003, see also Narayan et al 1997). …”

Section: Observational Features Consistent With the Jet Modelmentioning

confidence: 79%

Jet-dominated quiescent states in black hole X-ray binaries: the case of V404 Cyg

Xie

Yang

2014

Monthly Notices of the Royal Astronomical Society: Letters

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The dynamical structure and radiative properties of the quiescent state (X-ray luminosity 10 34 erg s −1 ) of black hole X-ray transients (BHXTs) remain unclear, mainly because of low luminosity and poor data quantity. We demonstrate that the simultaneous multi-wavelength (including radio, optical, ultraviolet and X-ray bands) spectrum of V404 Cyg in its bright quiescent state can be well described by the radiation from the companion star and more importantly, the compact jet. Neither the outer thin disc nor the inner hot accretion flow is important in the total spectrum. Together with recent findings, i.e. the power-law X-ray spectrum and the non-variable X-ray spectral shape (or constant photon index) in contrast to the dramatic change in the X-ray luminosity, we argue the quiescent state spectrum of BHXTs is actually jet-dominated. Additional observational properties consistent with this jet model are also discussed as supporting evidence.

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Section: Observational Features Consistent With the Jet Modelmentioning

confidence: 79%

Jet-dominated quiescent states in black hole X-ray binaries: the case of V404 Cyg

Xie

Yang

2014

Monthly Notices of the Royal Astronomical Society: Letters

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“…The same truncated thin disk scenario can also explain the low-frequency QPO. In the model proposed by Giannios & Spruit (2004;see also Rezzolla et al 2003 for a similar idea), the QPO arises from a global pmode oscillation of the hot ADAF. (As mentioned in Section 3.2.2, another QPO model invokes the precession of the ADAF, with the frequency again determined by the size of the ADAF.)…”

Section: Modeling Observations Of Bhbsmentioning

confidence: 95%

Hot Accretion Flows Around Black Holes

Yuan

Narayan

2014

Annu. Rev. Astron. Astrophys.

1,325

1,254

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Black hole accretion flows can be divided into two broad classes: cold and hot. Cold accretion flows, which consist of cool optically thick gas, are found at relatively high mass accretion rates. Prominent examples are the standard thin disk, which occurs at a fraction of the Eddington mass accretion rate, and the slim disk at super-Eddington rates. These accretion flows are responsible for luminous systems such as active galactic nuclei radiating at or close to the Eddington luminosity and black hole X-ray binaries in the soft state. Hot accretion flows, the topic of this review, are virially hot and optically thin. They occur at lower mass accretion rates, and are described by models such as the advection-dominated accretion flow and luminous hot accretion flow. Because of energy advection, the radiative efficiency of these flows is in general lower than that of a standard thin accretion disk. Moreover, the efficiency decreases with decreasing mass accretion rate. Observations show that hot accretion flows are associated with jets. In addition, theoretical arguments suggest that hot flows should produce strong winds. Hot accretion flows are believed to be present in low-luminosity active galactic nuclei and in black hole X-ray binaries in the hard and quiescent states. The prototype is Sgr A*, the ultra-low-luminosity supermassive black hole at our Galactic center. The jet, wind and radiation from a supermassive black hole with a hot accretion flow can interact with the external interstellar medium and modify the evolution of the host galaxy. Details of this "maintenance-mode feedback" could, in principle, be worked out through theoretical studies and numerical simulations of hot accretion flows.Comment: 69 pages, 9 figures; to appear in Annual Reviews of Astronomy and Astrophysics (2014

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“…It is therefore conceivable that radial pressure gradients may be important in trapping modes, and various groups have recently explored the possibility that accretion tori may explain observed QPO's, e.g. Giannios & Spruit (2004) for low‐frequency QPO's; Rezzolla et al (2003a), Kluźniak et al (2004) and Lee, Abramowicz & Kluźniak (2004) for high‐frequency QPO's. Geometrically thick tori may form in stellar collapse, and modes of dense tori around black holes have also been suggested as a detectable source of gravitational waves (e.g.…”

Section: Introductionmentioning

confidence: 99%

Oscillation modes of relativistic slender tori

Blaes

Arras

Fragile

2006

Monthly Notices of the Royal Astronomical Society

129

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Accretion flows with pressure gradients permit the existence of standing waves which may be responsible for observed quasi-periodic oscillations (QPO's) in X-ray binaries. We present a comprehensive treatment of the linear modes of a hydrodynamic, non-self-gravitating, polytropic slender torus, with arbitrary specific angular momentum distribution, orbiting in an arbitrary axisymmetric spacetime with reflection symmetry. We discuss the physical nature of the modes, present general analytic expressions and illustrations for those which are low order, and show that they can be excited in numerical simulations of relativistic tori. The mode oscillation spectrum simplifies dramatically for near Keplerian angular momentum distributions, which appear to be generic in global simulations of the magnetorotational instability. We discuss our results in light of observations of high frequency QPO's, and point out the existence of a new pair of modes which can be in an approximate 3:2 ratio for arbitrary black hole spins and angular momentum distributions, provided the torus is radiation pressure dominated. This mode pair consists of the axisymmetric vertical epicyclic mode and the lowest order axisymmetric breathing mode.Comment: submitted to MNRA

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Excitation of low-frequency QPOs in black hole accretion

Cited by 27 publications

References 46 publications

Jet-dominated quiescent states in black hole X-ray binaries: the case of V404 Cyg

Jet-dominated quiescent states in black hole X-ray binaries: the case of V404 Cyg

Hot Accretion Flows Around Black Holes

Oscillation modes of relativistic slender tori

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