Fast variability as a probe of the smallest regions around accreting black holes

Abstract

We extract the spectra of the fastest variability (above 10 Hz) from the black hole XTE J1550-564 during a transition from hard to soft state on the rise to outburst. We confirm previous results that the rapid variability contains no significant disc component despite this being strongly present in the total spectrum of the softer observations. We model ionised reflection significantly better than previous work, and show that this is also suppressed in the rapid variability spectrum compared to the total emission. This is consistent with the fast variability having its origin in a hot inner flow close to the black hole rather than in the accretion disc or in a corona above it. However, the rapid variability spectrum is not simply the same as the total Comptonised emission. It is always significantly harder, by an amount which increases as the spectrum softens during the outburst. This adds to evidence from time lags that the Comptonisation region is inhomogeneous, with harder spectra produced closest to the black hole, the same region which produces the fastest variability.

8 pages, 6 figures, to be published in MNRAS. Updated to match accepted version (smaller revisions)

References in corpus (4)

• Modelling the behaviour of accretion flows in X-ray binaries
• Hot accretion flow in black hole binaries: a link connecting X-rays to the infrared
• Spectral and Fourier analyses of X-ray QPO in accreting black holes
• High-frequency X-ray variability as a mass estimator of stellar and supermassive black holes

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