Relativistic and Newtonian diskoseismology

Wagoner, Robert V.

doi:10.1016/j.newar.2008.03.012

Cited by 21 publications

(28 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…I also show that a similar property holds for the QPOs predicted by the diskoseismology (see Ref. [51] for a review) and resonance [47,48] models.…”

Section: Introductionsupporting

confidence: 62%

X-ray probes of black hole accretion disks for testing the no-hair theorem

Johannsen¹

2014

Phys. Rev. D

View full text Add to dashboard Cite

The spins of a number of supermassive and stellar-mass black holes have been measured based on detections of thermal continuum emission and relativistically broadened iron lines in their x-ray spectra. Likewise, quasiperiodic variability has been observed in several sources. Such measurements commonly make the assumption that black holes are described by the Kerr metric, which according to the no-hair theorem characterizes black holes uniquely in terms of their masses and spins. This fundamental property of black holes can be tested observationally by measuring potential deviations from the Kerr metric introduced by a parametrically deformed Kerr-like spacetime. Thermal spectra, iron lines, and variability have already been studied extensively in several such metrics, which usually depend on only one particular type of deviation or contain unphysical regions outside of the compact object. In this paper, I study these x-ray probes in the background of a new Kerr-like metric which depends on four independent deviation functions and is free of pathological regions outside of the event horizon. I show that the observed signals depend significantly on primarily two types of deviations and that the strong correlation between the spin and the deviation parameters found previously in other Kerr-like metrics is partially broken for rapidly spinning black holes. This suggests that high-spin sources are the best candidates for tests of the no-hair theorem with x-rays and I obtain first constraints on such deviations from the stellar-mass black hole Cygnus X-1.

show abstract

“…I also show that a similar property holds for the QPOs predicted by the diskoseismology (see Ref. [51] for a review) and resonance [47,48] models.…”

Section: Introductionsupporting

confidence: 62%

X-ray probes of black hole accretion disks for testing the no-hair theorem

Johannsen¹

2014

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…Physical origins of the HFQPOs are highly debated. Models are often based on an ISCO orbital frequency, an epicyclic frequency, and frequencies of various pressure and gravity modes (e.g., Kato 2001Kato , 2004Remillard & McClintock 2006;Wagoner 2008). The underlying physics involves beat oscillations (van der Klis 2000), resonances between flow modes and normal frequencies in general relativity (GR) (Abramowicz & Kluźniak 2001), trapped oscillations (Nowak & Wagoner 1991), parametric resonances (Abramowicz et al 2003), and disk magnetospheric oscillations (Li & Narayan 2004).…”

Section: Introductionmentioning

confidence: 99%

SUBMILLIMETER QUASI-PERIODIC OSCILLATIONS IN MAGNETICALLY CHOKED ACCRETION FLOW MODELS OF SgrA*

Shcherbakov

McKinney

2013

ApJ

View full text Add to dashboard Cite

High-frequency quasi-periodic oscillations (QPOs) appear in general-relativistic magnetohydrodynamic simulations of magnetically choked accretion flows around rapidly rotating black holes (BHs). We perform polarized radiative transfer calculations with ASTRORAY code to explore the manifestations of these QPOs for SgrA*. We construct a simulation-based model of a radiatively inefficient accretion flow and find model parameters by fitting the mean polarized source spectrum. The simulated QPOs have a total sub-mm flux amplitude up to 5% and a linearly polarized flux amplitude up to 2%. The oscillations reach high levels of significance 10 − 30σ and high quality factors Q ≈ 5. The oscillation period T ≈ 100M ≈ 35 min corresponds to the rotation period of the BH magnetosphere that produces a trailing spiral in resolved disk images. The total flux signal is significant over noise for all tested frequencies 87 GHz, 230 GHz, and 857 GHz and inclination angles 10 • , 37 • , and 80 • . The non-detection in the 230 GHz Sub-Millimeter Array light curve is consistent with a low signal level and a low sampling rate. The presence of sub-mm QPOs in SgrA* will be better tested with the Atacama Large Millimeter Array.

show abstract

“…These ideas have been widely discussed and adapted into numerous individual disc-oscillation models. The subject of disc oscillations and their propagation has been extensively studied analytically for thin disc (i.e., nearly geodesic, radiatively efficient) configurations (Okazaki et al 1987;Kato et al 1998;Wagoner 1999Wagoner , 2008Wagoner et al 2001;Silbergleit et al 2001;Ortega-Rodríguez et al 2002). The derived results have been compared to those for "thick" (radiatively inefficient, slim-disc or toroidal) configurations foe which both analytical (Blaes 1985;Šrámková 2005;Abramowicz et al 2006;Blaes et al 2006Blaes et al , 2007Straub & Šrámková 2009) and numerical (Rezzolla et al 2003a,b;Rezzolla 2004;Montero et al 2004;Zanotti et al 2005;Šrámková et al 2007) studies have been performed.…”

Section: Hf Qpo Interpretationmentioning

confidence: 99%

Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model

Urbanec

Török

Šrámková

et al. 2010

A&A

View full text Add to dashboard Cite

The high-frequency quasi-periodic oscillations (HF QPOs) that appear in the X-ray fluxes of low-mass X-ray binaries remain an unexplained phenomenon. Among other ideas, it has been suggested that a non-linear resonance between two oscillation modes in an accretion disc orbiting either a black hole or a neutron star plays a role in exciting the observed modulation. Several possible resonances have been discussed. A particular model assumes resonances in which the disc-oscillation modes have the eigenfrequencies equal to the radial and vertical epicyclic frequencies of geodesic orbital motion. This model has been discussed for black hole microquasar sources as well as for a group of neutron star sources. Assuming several neutron (strange) star equations of state and Hartle-Thorne geometry of rotating stars, we briefly compare the frequencies expected from the model to those observed. Our comparison implies that the inferred neutron star radius R NS is larger than the related radius of the marginally stable circular orbit r ms for nuclear matter equations of state and spin frequencies up to 800 Hz. For the same range of spin and a strange star (MIT) equation of state, the inferrred radius is R NS ∼ r ms . The "Paczyński modulation" mechanism considered within the model requires that R NS < r ms . However, we find this condition to be fulfilled only for the strange matter equation of state, masses below 1 M , and spin frequencies above 800 Hz. This result most likely falsifies the postulation of the neutron star 3:2 resonant eigenfrequencies being equal to the frequencies of geodesic radial and vertical epicyclic modes. We suggest that the 3:2 epicyclic modes could stay among the possible choices only if a fairly non-geodesic accretion flow is assumed, or if a different modulation mechanism operates.

show abstract

Relativistic and Newtonian diskoseismology

Cited by 21 publications

References 11 publications

X-ray probes of black hole accretion disks for testing the no-hair theorem

X-ray probes of black hole accretion disks for testing the no-hair theorem

SUBMILLIMETER QUASI-PERIODIC OSCILLATIONS IN MAGNETICALLY CHOKED ACCRETION FLOW MODELS OF SgrA*

Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model

Contact Info

Product

Resources

About