A precise determination of black hole spin in GRO J1655-40

By Marek Abramowicz, W. Kluźniak. 2001

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We note that the recently discovered 450 Hz frequency in the X-ray flux of the black hole candidate GRO J1655-40 is in a 3:2 ratio to the previously known 300 Hz frequency of quasi-periodic oscillations (QPO) in the same source. If the origin of high frequency QPOs in black hole systems is a resonance between orbital and epicyclic motion of accreting matter, as suggested previously, the angular momentum of the black hole can be accurately determined, given its mass. We nd that the dimensionless angular momentum is in the range 0:2 <j< 0:67 if the mass is in the (corresponding) range of 5.5 to 7.9 solar masses.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/427e983d8acfb63e132a33c49a35932bbea80ea9

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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 frequency ratio 3:2 (or other rational ratios as 3:1 or 2:1) of the observed twin frequencies in microquasars indicate resonance phenomena at work [104,108].”
The orbital resonance model for twin peak kHz quasi periodic oscillations in microquasars (2005, background): “It was realized (Abramowicz & Kluźniak 2001; Kluźniak & Abramowicz 2002; McClintock & Remillard 2003; see also Table 1 and its references) that typically the two frequencies, νupp, νdown, form rational ratios and that most often νupp/νdown = 3/2.”
A review of quasi-periodic oscillations from black hole X-ray binaries: Observation and theory (2019, background): “Since HF QPOs have frequencies commensurate with the epicyclic frequencies of particle motion close to the innermost stable circular orbit (ISCO) of the BH, they have been the subject of great theoretical interest [1, 107].”
Orbital resonances in discs around braneworld Kerr black holes (2008, methodology): “here even the case with νK(x,a,b)=νθ(x,a,b)=νr(x,a,b)is possible (where the lines arsr (x,b) and aθ sr(x,b) cross each other). 6 Resonance conditions The orbital resonance models for QPOs proposed in [4,5] are particularly based on resonance between oscillations with the epicyclic frequencies which ”
Evidence for Harmonic Relationships in the High-Frequency Quasi-periodic Oscillations of XTE J1550–564 and GRO J1655–40 (2002, background): “For GRO J1655 40, Abramowicz & Kluzniak (2001) constrain the spin parameter to the range 0:2 a 0:67 for a black hole mass in the range 5.5–7.9 M .”
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).”