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We propose a physical model for the peaked noise in the X-ray power densityspectra of accreting X-ray binaries. We interpret its appearance as aninterference of two Comptonization continua: one coming from the up-scatteringof seed photons from the cold thin disk and the other fed by the synchrotronemission of the hot flow. Variations of both X-ray components are caused byfluctuations in mass accretion rate, but there is a delay between themcorresponding to the propagation timescale from the disk Comptonization radiusto the region of synchrotron Comptonization. If the disk and synchrotronComptonization are correlated, the humps in the power spectra are harmonicallyrelated and the dips between them appear at frequencies related as odd numbers1:3:5. If they are anti-correlated, the humps are related as 1:3:5, but thedips are harmonically related. Similar structures are expected to be observedin accreting neutron star binaries and supermassive black holes. The delay canbe easily recovered from the frequency of peaked noise and further used toconstrain the combination of the viscosity parameter and disk height-to-radiusratio $\alpha (H/R)^2$ of the accretion flow. We model multi-peak power spectraof black hole X-ray binaries GX 339$-$4 and XTE J1748$-$288 to constrain theseparameters.

Interference as an origin of the peaked noise in accreting X-ray binaries