X-ray QPOs from Black Hole Binary Systems

Details X-ray QPOs from Black Hole Binary Systems X-ray QPOs from Black Hole Binary Systems

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..714...13r&link_type=abstract

X-RAY TIMING 2003: Rossie and Beyond. AIP Conference Proceedings, Volume 714, pp. 13-20 (2004).

Astronomy and Astrophysics

Astrophysics

13

X- And Gamma-Ray Telescopes And Instrumentation, Spaceborne And Space Research Instruments, Apparatus, And Components, X-Ray

Scientific paper

X-ray QPOs from black hole binary systems provide specialized and extraordinary tools for black-hole astrophysics. Low-frequency QPOs (LFQPOs 0.1-30 Hz) help us to distinguish black hole spectral states, which are now understood in terms of radiation dominance by either the accretion disk, a jet, or a compact high-energy corona. LFQPOs can be remarkably strong (rms > 20% at 2-30 keV) and coherent (Q > 10) in the ``steep power-law'' state, and this imposes first-order requirements for physical models for the compact corona that powers this state. Strong LFQPOs can also be seen in the hard state (radio-loud, steady jet), particularly when the energy spectrum shows a mixture of thermal and hard power-law components. In several sources, correlations have been found between LFQPO frequency and either the integrated thermal flux or the power-law spectral index. This provides further evidence that LFQPO oscillations are tied to the energy coupling between the disk and either the jet or the compact corona.
High-frequency QPOs (HFQPOs 40-450 Hz) are transient and subtle (rms amplitudes near 1%), and most detections occur in the steep power-law state. Three (possibly four) sources exhibit HFQPOs that primarily represent a pair of commensurate frequencies in a 3:2 ratio, with detections that cover a wide range in luminosity. Furthermore, the three pairs of QPOs appear to represent fixed frequency systems that scale inversely with black hole mass. These results provide strong encouragement to investigate HFQPOs as some type of resonance oscillation rooted in general relativity. A successful determination of the correct oscillation mechanism would yield invaluable measurement constraints on black hole mass and spin.

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