Quasi-periodic Oscillations in the X-Ray Light Curves from Relativistic Tori

Schnittman, Jeremy D.; Rezzolla, Luciano

doi:10.1086/500545

Cited by 55 publications

(67 citation statements)

References 24 publications

(36 reference statements)

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“…and Schnittman & Rezzolla (2006), gravitational redshifts, Doppler shifts, and lensing of X-ray photons emitted by tori oscillating in both the vertical and radial epicyclic modes can produce detectable oscillations in the predicted X-ray fluxes measured by an observer.…”

Section: Discussionmentioning

confidence: 94%

Epicyclic Oscillations of Fluid Bodies: Newtonian Nonslender Torus

Blaes

Šrámková

Abramowicz

et al. 2007

ApJ

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We study epicyclic oscillations of fluid tori around black holes (in the Paczyński-Wiita potential) and derive exact analytic expressions for their radial and vertical eigenfrequencies r and z to second-order accuracy in the width of the torus. We prove that pressure effects make the eigenfrequencies smaller than those for free particles. However, the particular ratio z / r ¼ 3/2, which is important for the theory of high-frequency quasi-periodic oscillations (QPOs), occurs when the fluid tori epicyclic frequencies r and z are about 15% higher than the ones corresponding to free particles. Our results therefore suggest that previous estimates of black hole spins from QPOs have produced values that are too high.

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Section: Discussionmentioning

confidence: 94%

Epicyclic Oscillations of Fluid Bodies: Newtonian Nonslender Torus

Blaes

Šrámková

Abramowicz

et al. 2007

ApJ

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“…If that is correct, they may be used to probe the geometry around stellar-mass BH candidates. For the time being, however, the exact physical mechanism responsible for the production of the high-frequency QPOs is not known and several different scenarios have been proposed, including hot-spot models (Stella & Vietri 1998, diskoseismology models (Perez et al 1997;Silbergleit et al 2001;Wagoner et al 2001;Kato 2001), resonance models (Abramowicz & Kluzniak 2001;Abramowicz et al 2003;Kluzniak & Abramowicz 2005;Török et al 2005), and p-mode oscillations of a small accretion torus (Rezzolla et al 2003a,b;Schnittman & Rezzolla 2006). In these models, the frequencies of the QPOs are directly related to the three characteristic orbital frequencies of a test-particle: the Keplerian frequency ν K (which is the inverse of the orbital period), the radial epicyclic frequency ν r (the frequency of radial oscillations around the mean orbit), and the vertical epicyclic frequency ν θ (the frequency of vertical oscillations around the mean orbit).…”

Section: Quasi Periodic Oscillationsmentioning

confidence: 99%

Testing the space-time geometry around black hole candidates with the available radio and X-ray data

Bambi

2013

Astronomical Review

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Astrophysical black hole candidates are thought to be the Kerr black holes predicted by General Relativity, but the actual nature of these objects has still to be proven. The Kerr black hole hypothesis can be tested by observing strong gravity features and check if they are in agreement with the predictions of General Relativity. In particular, the study of the properties of the electromagnetic radiation emitted by the gas of the accretion disk can provide information on the geometry of the space-time around these objects and constrain possible deviations from the Kerr background.

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“…How does this assumption affect the results that we have obtained? Studies (see Schnittman & Bertschinger 2004;Broderick & Loeb 2005;Schnittman & Rezzolla 2006;Yang & Wang 2013;Li et al 2014), indicate that the spectrograms and lightcurves from an emitting plasma blob in the vicinity of a black hole are weakly dependent on the size of the emitter. However, a finite-size plasmoid near a black hole will subject to a strong tidal force, which will cause it to deform over the course of its orbital motion around the black hole.…”

Section: Dynamics Of Plasmoid Ejectionmentioning

confidence: 99%

Variations in emission from episodic plasmoid ejecta around black holes

Younsi¹,

Wu²

2015

Mon. Not. R. Astron. Soc.

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The X-ray and radio flares observed in X-ray binaries and active galactic nuclei (AGN) are attributed to energetic electrons in the plasma ejecta from the accretion flows near the black hole in these systems. It is argued that magnetic reconnection could occur in the coronae above the accretion disk around the black hole, and that this drives plasmoid outflows resembling the solar coronal mass ejection (CME) phenomenon. The X-ray and radio flares are emission from energetic electrons produced in the process. As the emission region is located near the black hole event horizon, the flare emission would be subject to special-and general-relativistic effects. We present calculations of the flaring emission from plasmoids orbiting around a black hole and plasmoid ejecta launched from the inner accretion disk when general-relativistic effects are crucial in determining the observed time-dependent properties of the emission. We consider fully general-relativistic radiative transfer calculations of the emission from evolving ejecta from black hole systems, with proper accounting for differential arrival times of photons emitted from the plasmoids, and determine the emission lightcurves of plasmoids when they are in orbit and when they break free from their magnetic confinement. The implications for interpreting time-dependent spectroscopic observations of flaring emission from accreting black holes are discussed.

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Quasi-periodic Oscillations in the X-Ray Light Curves from Relativistic Tori

Cited by 55 publications

References 24 publications

Epicyclic Oscillations of Fluid Bodies: Newtonian Nonslender Torus

Epicyclic Oscillations of Fluid Bodies: Newtonian Nonslender Torus

Testing the space-time geometry around black hole candidates with the available radio and X-ray data

Variations in emission from episodic plasmoid ejecta around black holes

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