Here we used numerical simulations based on ray-tracing method in Kerr metric to study the influence of strong gravity and spin of supermassive black holes on radiation emitted from their relativistic accretion disks. The obtained results showed that space-time metric has a significant influence on the shape of the broad Fe Kα spectral line, emitted from the innermost parts of such relativistic accretion disks. These simulations, when compared with the observed X-ray spectra of active galaxies and quasars, could be used for obtaining the parameters of their central supermassive black holes (e.g. their spins) and for studying the plasma physics, space-time geometry and effects of strong gravity in the central parts of these objects.
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