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Fig. 1.

image

Geometry of our model. The accretion disc varies on long timescales and extends from 400rgrtrc. The inner regions from rtrcrsh and rsh–1.23rg are turbulent inner flows varying intrinsically on fast timescales that are responsible for the soft and hard spectral emission, respectively. The accretion disc provides seed photons to the inner hot flows, and reprocesses and reflects the Comptonized emission photons coming back from the inner regions. The parameter tp is the time taken for fluctuations to propagate from rtrc to rsh.

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