Basic Properties of Thin-Disk Oscillations

By S. Kato. 2001

227 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/e591132f14f1b6ffe87822fd172ccab1e98c100c

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Citations in the corpus

Non-Linear Resonance in Nearly Geodesic Motion in Low-Mass X-Ray Binaries (2003, unknown): “These black-hole QPOs are thought to have stable frequencies, and until the discovery of the puzzling rational ratios they have been thought to correspond to a trapped g-mode or c-mode of disc oscillation in the Kerr metric (Okazaki et al. 1987; Wagoner 1999; Wagoner et al. 2001; Kato 2001).”
No observational proof of the black-hole event-horizon (2002, background): “…that of a rotating star (if no star can be the “source” of the a , 0 Kerr metric, see Abramowicz et al. 1976), is through the study of orbital and other frequencies (e.g., epicyclic) of accreting matter moving in strong-field gravity (Kato 2001; Wagoner 2001; Abramowicz & Kluźniak 2001, 2002).”
Multi-resonance orbital model of high-frequency quasi-periodic oscillations: possible high-precision determination of black hole and neutron star spin (2013, background): “…the oscillatory motion of hot spots or accretion disc oscillations, such as the total precession model (Stuchlík et al. 2007d), the tidal disruption model (̌Cadež et al. 2008; Kostić et al. 2009; Germanà et al. 2009), or the warped disc oscillations model (Kato 2001a, 2004b,a, 2007, 2008, 2009).”
X-Ray Properties of Black-Hole Binaries (2006, background): “As shown in Figure 12, their frequencies appear to scale inversely with mass (McClintock & Remillard 2006), which is the dependence expected for coordinate frequencies (see Merloni et al. 1999) or for diskoseismic modes in the inner accretion disk (Wagoner 1999; Kato 2001).”
Evidence for Harmonic Relationships in the High-Frequency Quasi-periodic Oscillations of XTE J1550–564 and GRO J1655–40 (2002, methodology): “Unlike the orbital and polar frequencies, the radial coordinate frequency reaches a maximum value at a radius larger than the innermost stable orbit, regardless of the values of black hole mass and spin (see Kato 2001; Merloni et al. 1999; and references therein).”
A new simple model for high-frequency quasi-periodic oscillations in black hole candidates (2003, unknown): “The predictions of the model are well summarised by Kato (2001).”
A precise determination of black hole spin in GRO J1655-40 (2001, background): “The formulae for the frequencies can be found, e.g., in the review by Kato (2001) and references therein.”
A review of quasi-periodic oscillations from black hole X-ray binaries: Observation and theory (2019, background): “ped in a region between the disc inner radius r in and another radius called the inner vertical resonance (IVR) r ivr, and excited by perturbations in an intrinsic disc quantity such as density (e.g. [108, 249, 106]). Visualisations of such oscillations can be found in Fig 2 of Tsang and Butsky [228”