High-frequency QPOs as a problem in physics: non-linear resonance

Kluźniak, W.; Abramowicz, Marek A.; Lee, William H.

doi:10.1063/1.1781058

Cited by 9 publications

(3 citation statements)

References 11 publications

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“…In refs. [14,15], and in these Proceedings [16], we discuss a resonance in an accretion disk or torus excited by an external forcing by a millisecond pulsar. A similar forcing is crucially important in a different, non-relativistic resonance model suggested by Titarchuk [17].…”

Section: Introductionmentioning

confidence: 99%

Interpreting black hole QPOs

Abramowicz

Kluźniak

2004

AIP Conference Proceedings

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In all the microquasars with two hHz QPOs, the ratio of the frequencies is 3:2, supporting our suggestion that a non-linear resonance between two modes of oscillation in the accretion disk plays a role in exciting the observed modulations of the X-ray flux. We discuss the evidence in favor of this interpretation, and we relate the black hole spin to the frequencies expected for various types of resonances that may occur in nearly Keplerian disks in strong gravity. For those microquasars where the mass of the central X-ray source is known, the black hole spin can be deduced from a comparison of the observed and expected frequencies.Comment: Invited lecture: X-Ray Timing 2003: Rossi and Beyond (Harvard, 2003

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Section: Introductionmentioning

confidence: 99%

Interpreting black hole QPOs

Abramowicz

Kluźniak

2004

AIP Conference Proceedings

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“…Currently, the main interest in disk oscillations is related to the observed frequencies in the X-ray flux from black hole and neutron star systems (for a review see van der Klis M., 2000). For black hole disks the modes thought to be offering the most promising explanation (Wagoner et al, 2001) of the highest observed frequencies are the g-modes and c-modes, investigated in full GR by Perez et al (1997); Silbergleit et al (2001), although a different explanation seems to be required for the observed 3:2 ratio of the highest frequencies in the microquasars (Abramowicz and Kluźniak, 2001;Kluźniak et al, 2004;Török et al, 2005). Thus, the modes investigated here are not prime candidates for a theoretical counterpart to the observed high frequency QPOs (quasi-periodic oscillations) in black hole systems.…”

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confidence: 99%

Eigenmodes of trapped horizontal oscillations in accretion disks

Khanna,

Strzelecka,

Mishra

et al. 2014

Preprint

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We present eigenfrequencies and eigenfunctions of trapped acoustic-inertial oscillations of thin accretion disks for a Schwarzschild black hole and a rapidly rotating Newtonian star (a Maclaurin spheroid). The results are derived in the formalism of Nowak and Wagoner (1991) with the assumption that the oscillatory motion is parallel to the midplane of the disk. The first four radial modes for each of five azimuthal modes (m = 0 through m = 4) are presented. The frequencies and wavefunctions of the lowest modes may be accurately approximated by Airy's function.

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“…The oscillations could be related to both the thin Keplerian discs [9,10] or the thick, toroidal accretion discs [11,12]. The parametric resonance of the radial and vertical oscillations in the thin discs can explain the QPOs with the ω θ /ω r = 3 : 2 frequency ratio observed in all the microquasars and can put strong limits on the rotational parameter of their central black holes related to the limits on their mass [13].…”

Section: Introductionmentioning

confidence: 99%

Toroidal LNRF-velocity profiles in thick accretion discs orbiting rapidly rotating Kerr black holes

Stuchlík¹,

Slaný²,

Török³

2006

AIP Conference Proceedings

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Abstract. We show that in the equatorial plane of marginally stable thick discs (with uniformly distributed specific angular momentum ℓ(r, θ ) = const) the orbital velocity relative to the LNRF has a positive radial gradient in the vicinity of black holes with a > 0.99979. The change of sign of the velocity gradient occurs just above the center of the thick toroidal discs, in the region where stable circular geodesics of the Kerr spacetime are allowed. The global character of the phenomenon is given in terms of topology changes of the von Zeipel surfaces (equivalent to equivelocity surfaces in the tori with ℓ(r, θ ) = const). Toroidal von Zeipel surfaces exist around the circle corresponding to the minimum of the equatorial LNRF velocity profile, indicating a possibility of development of some vertical instabilities in those parts of marginally stable tori with positive gradient of the LNRF velocity. Eventual oscillatory frequencies connected with the phenomenon are given in a coordinateindependent form.

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High-frequency QPOs as a problem in physics: non-linear resonance

Cited by 9 publications

References 11 publications

Interpreting black hole QPOs

Interpreting black hole QPOs

Eigenmodes of trapped horizontal oscillations in accretion disks

Toroidal LNRF-velocity profiles in thick accretion discs orbiting rapidly rotating Kerr black holes

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