Abstract
Recent observations of galactic bulge X-ray sources have revealed in some cases the existence of a hot accretion disk corona1,2 and in others quasi-periodic oscillations (QPOs) in the X-ray flux3–5. We suggest here that these properties are directly related and that the oscillations are produced in the innermost parts of the corona. The observed variations in the centroid frequency of the QPOs with source intensity3–6 are explained and further variations with the photon spectrum predicted. Unlike some alternative models7,8, we do not require that the central object is a rapidly spinning weakly magnetized neutron star.
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