A new simple model for high-frequency quasi-periodic oscillations in black hole candidates

By Luciano Rezzolla, S. Yoshida, T. Maccarone, Olindo Zanotti. 2003

236 citations recorded by the source corpus.

Observations of X-ray emissions from binary systems have long since been considered important tools to test general relativity in strong-field regimes. The high-frequency quasi-periodic oscillations (HFQPOs) observed in binaries containing a black hole candidate, in particular, have been proposed as a means to measure more directly the properties of the black hole, such as its mass and spin. Numerous models have been suggested to explain the HFQPOs and the rich phenomenology accompanying them. Many of these models rest on a number of assumptions and are at times in conflict with the most recent observations. We here propose a new, simple model in which the HFQPOs result from basic p-mode oscillations of a small accretion torus orbiting close to the black hole. We show that within this model the key properties of the HFQPOs can be explained simply, given a single reasonable assumption. We also discuss observational tests that can refute the model.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/aa2035d0caa03578146163b90cb77c2edd626249

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Citations in the corpus

Testing Accretion Disk Theory in Black Hole X-Ray Binaries (2006, background): “For example, if the lower frequency member of the pair in J1550 and J1655 is identified as an axisymmetric radial epicyclic oscillation, then black hole spins of a∗ > 0.9 are required (Rezzolla et al. 2003, Török 2005).”
Modelling the behaviour of accretion flows in X-ray binaries (2007, background): “Further investigations, looking at modes of this hot flow (Rezzolla et al 2003; Giannos & Spruit 2004; Blaes, Fragile & Arras 2006) and how it interacts with the surface should surely give insights into these remaining issues.”
An Accretion-Jet Model for Black Hole Binaries: Interpreting the Spectral and Timing Features of XTE J1118+480 (2004, background): “For example, Giannios & Spruit (2004; see also Rezzolla et al. 2003) suggest that the QPO can be excited by the interaction of the inner hot accretion flow and outer thin disk.”
TESTING THE NO-HAIR THEOREM WITH OBSERVATIONS IN THE ELECTROMAGNETIC SPECTRUM. IV. RELATIVISTICALLY BROADENED IRON LINES (2012, result): “Similar conclusions can be reached for other QPO models, e.g., Kluźniak & Abramowicz (2001); Abramowicz et al. (2003); Rezzolla et al. (2003).”
Hot Accretion Flows Around Black Holes (2014, result): “In the model proposed by Giannios & Spruit (2004; see also Rezzolla et al. 2003 for a similar idea), the QPO arises from a global p-mode oscillation of the hot ADAF.26 The QPO frequency is roughly determined by the Keplerian frequency at Rtr and agrees well with the observed frequency for Rtr ≈…”
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).”
X-Ray Properties of Black-Hole Binaries (2006, background): “In an alternative model, state changes are invoked that thicken the inner disk into a torus; the normal modes (with or without a resonance condition) can yield oscillations with a 3:2 frequency ratio (Rezzolla et al. 2003; Fragile 2005).”
Multi-resonance orbital model of high-frequency quasi-periodic oscillations: possible high-precision determination of black hole and neutron star spin (2013, background): “…star (massM, spina, and quadrupole momentq in the case of neutron stars).2 The frequencies of disc oscillation modes can be 2 For toroidal discs (Rezzolla et al. 2001, 2003b; Blaes et al.2007; Straub & Šrámková 2009; Montero & Zanotti 2012) or slightly charged discs around magnetic neutron…”