“Stable” Quasi-periodic Oscillations and Black Hole Properties from Diskoseismology

Wagoner, Robert V.; Silbergleit, A. S.; Ortega‐Rodríguez, Manuel

doi:10.1086/323655

Cited by 189 publications

(189 citation statements)

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“…Note that, although the 1:4 ratio is unconventional, it follows for instance from the discoseismic model ( [33] and references therein) as a combination between a g-and c-mode oscillation or as a non-axisymmetric oscillation between two gmodes [33]. Also, in the model by Abromowicz and Kluźniak it is perhaps possible to get a 1:4 ratio by putting the ratio between the relativistic epicyclic frequency and the relativistic Keplerian frequency equal to 1:4.…”

Section: Discussionmentioning

confidence: 99%

High frequency features in the 1998 outburst of 4U 1630–47

Klein-Wolt

Homan

Klis

2004

Nuclear Physics B - Proceedings Supplements

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Section: Discussionmentioning

confidence: 99%

High frequency features in the 1998 outburst of 4U 1630–47

Klein-Wolt

Homan

Klis

2004

Nuclear Physics B - Proceedings Supplements

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“…A different model that warrants consideration with respect to harmonic HFQPOs in black hole binaries is the diskoseismic model (Kato & Fukue 1980;Wagoner 1999;Kato 2001;Wagoner et al 2001). Here GR theory predicts that the inner accretion disk may trap oscillations, which is a consequence related to the turnover in the radial coordinate frequency at small radii, which was noted previously.…”

Section: Diskoseismic Oscillation Modelsmentioning

confidence: 99%

Evidence for Harmonic Relationships in the High‐Frequency Quasi‐periodic Oscillations of XTE J1550−564 and GRO J1655−40

Remillard

Muno

McClintock

et al. 2002

ApJ

193

293

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We continue to investigate the X-ray properties of the black hole binary XTE J1550À564. By grouping observations (1998)(1999) according to the type of low-frequency quasiperiodic oscillation (LFQPO) identified in a previous paper, we show evidence that two high-frequency QPOs (HFQPOs) occur simultaneously near 184 and 276 Hz. We can model the QPO profiles while assuming that the central frequencies are related by a 3 : 2 ratio. In one group, there is some evidence of a broad feature at the fundamental frequency of 92 Hz. We also investigate the 2000 April outburst, and we confirm the suggestion of Miller et al. that a 270 Hz QPO is accompanied by a second feature near 180 Hz. The histogram for the 28 individual HFQPO detections in XTE J1550À564 shows two peaks near 184 and 276 Hz, while there is a notable exception in the 143 Hz QPO detected on 1998 October 15. Similarly, all of the 13 HFQPO detections in the black hole binary GRO J1655À40 occur at two frequencies that are related by a 3 : 2 ratio. We next investigate all of the energy spectra for XTE J1550À564, and we find a systematic increase in the strength of the power-law component as the stronger of the two HFQPOs shifts from 276 to 184 Hz. A strikingly similar result is seen in the spectra of GRO J1655À40 when the stronger HFQPO shifts from 450 to 300 Hz. The fundamental HFQPO frequencies for the two X-ray sources scale as M À1 , which is consistent with the hypotheses that these HFQPOs represent some kind of oscillation rooted in general relativity (GR) and that the two black holes have similar values of the dimensionless spin parameter. We discuss physical mechanisms that may explain these HFQPOs. A resonance between orbital and radial coordinate frequencies is one possibility suggested by Abramowicz & Kluzniak. For XTE J1550À564, this would imply moderate values for the dimensionless spin parameter (0:1 < a Ã < 0:6), with similar results for GRO J1655À40. A resonance between polar and radial coordinate frequencies allows additional values for a * above 0.9. There remain serious uncertainties regarding the physical mechanism whereby resonances in coordinate frequencies may produce HFQPOs. We also discuss models for '' diskoseismic '' oscillations. In this case, the concept that the inner disk behaves as a resonance cavity in GR has certain attractions for explaining HFQPOs, but integral harmonics are not predicted for the three types of diskoseismic modes derived for adiabatic perturbations in a thin accretion disk.

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“…Although there is great debate as to the correct model for these oscillations, there is a general consensus that the high, stable frequencies point towards a direct relationship to the gravity of the black hole in the "strong field" regime of GR. The oscillations therefore may act as independent probes of black hole mass and spin [295][296][297][298][299]. It is hoped that models of variability can be combined with models of broadened lines to yield even tighter constraints on black hole mass and spin.…”

Section: Other Gbhc and Spectral Correlationsmentioning

confidence: 99%