Interpreting black hole QPOs

Abstract

In all the microquasars with two hHz QPOs, the ratio of the frequencies is 3:2, supporting our suggestion that a non-linear resonance between two modes of oscillation in the accretion disk plays a role in exciting the observed modulations of the X-ray flux. We discuss the evidence in favor of this interpretation, and we relate the black hole spin to the frequencies expected for various types of resonances that may occur in nearly Keplerian disks in strong gravity. For those microquasars where the mass of the central X-ray source is known, the black hole spin can be deduced from a comparison of the observed and expected frequencies.

Invited lecture: X-Ray Timing 2003: Rossi and Beyond (Harvard, 2003)

Cited by in corpus (15)

• A 400 solar mass black hole in the Ultraluminous X-ray source M82 X-1 accreting close to its Eddington limit
• Measuring mass and angular momentum of black holes with high-frequency quasi-periodic oscillations
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• Oscillations of tori in the pseudo-Newtonian potential
• Disc-oscillation resonance and neutron star QPOs: 3:2 epicyclic orbital model
• Difficulties with the QPOs Resonance Model
• Confronting models for the high-frequency QPOs with Lense-Thirring precession
• QPOs in Cataclysmic Variables and in X-ray Binaries
• Measurement of Mass and Spin of Black Holes with QPOs
• High-frequency QPOs as a problem in physics: non-linear resonance
• Quasiperiodic oscillations and Tomimatsu-Sato δ = 2 space-time
• QPOs in microquasars: the spin problem
• Tidal forces around the Letelier-Alencar cloud of strings black hole
• X-ray Timing beyond the Rossi X-ray Timing Explorer
• Mass-spin relation of black holes obtained by twin high-frequency quasi-periodic oscillations