The orbital resonance model for twin peak kHz quasi periodic oscillations in microquasars

By G. Török, Marek Abramowicz, W. Kluźniak, Zdenek Stuchlík. 2005

207 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Biomedical Engineering, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b34eeb4b3a44d45d9a94b235f55688c8a0823141

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Citations in the corpus

Influence of Cosmic Repulsion and Magnetic Fields on Accretion Disks Rotating around Kerr Black Holes (2020, background): “The most widely discussed are the epicyclic resonance [109] and the hot-spot relativistic precession [115] variants of the geodesic model, having simple identification of the twin observed frequencies (lower fL, and upper fU) with the frequencies of the variants of the geodesic model of twin HF QPOs”
X-Ray Properties of Black-Hole Binaries (2006, background): “For example, the “parametric resonance” concept (Abramowicz et al. 2003; Kluzńiak et al. 2004; Török et al. 2005) describes oscillations rooted in fluid flow where there is a coupling between the radial and polar coordinate frequencies.”
Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets (2013, methodology): “Two other methods for measuring the spins of stellar black holes appear promising, namely, via X-ray polarimetry (Dovˇciak et al. 2008; Li et al. 2009; Schnittman & Krolik 2009) and high-frequency quasiperiodic oscillations (T¨or¨ok et al. 2005; Remillard & McClintock 2006; Belloni et al. 2012).”
Testing black hole candidates with electromagnetic radiation (2015, background): “…been proposed, and in particular there are relativistic precession models (Motta et al., 2014; Stella & Vietri, 1999), diskoseismology models (Perez et al., 1997), resonance models (Abramowicz & Kluźniak, 2001; Török et al., 2005), p-mode oscillations of accretion tori (Rezzolla et al., 2003).”
Measuring the spins of accreting black holes (2011, methodology): “We note that spin estimates have also been obtained by modeling the high-frequency x-ray oscillations (100–450 Hz) observed for several stellar-mass black holes (Wagoner et al 2001, Török et al 2005).”
The Spin of the Near-Extreme Kerr Black Hole GRS 1915+105 (2006, background): “Presently, however, the leading model of HFQPOs, which was initially proposed by Abramowicz & Kluzńiak (2001), does not provide a useful constraint on a∗ for GRS1915 because of the wide range of possible resonances and the sizable uncertainty in the BH mass (Török et al. 2005).”
Relativistic X-Ray Lines from the Inner Accretion Disks Around Black Holes (2007, background): “An extremely skewed feature was recently reported in XMM-Newton spectra of GRO J1655−40, in which X-ray variability studies also find evidence for spin (see, e.g., Strohmayer 2001, Torok et al. 2005).”
Multi-resonance orbital model of high-frequency quasi-periodic oscillations: possible high-precision determination of black hole and neutron star spin (2013, methodology): “For any specific version of the orbital resonance models, the resonant radii at thin, Keplerian accretion discs (Török et al. 2005) are given by the frequency ratio and the parameters of the central black hole or neutron star (massM, spina, and quadrupole momentq in the case of neutron stars).2 The ”