Modeling the X‐ray variability in MCG‐6‐30‐15: the multiple flare model

We report on the current state of the multiple flare model that was developed to explain the observed X‐ray variability in active galactic nuclei. The method assumes temporary spots co‐rotating with the accretion disk. Here we apply the model to the 300 ksec XMM‐Newton observation of the Seyfert galaxy MCG‐6‐30‐15. We find a satisfying reproduction of the rms‐variability data at photon energies between 4 keV and 10 keV. The observed shape of the power spectral density, on the other hand, remains difficult to explain by a model of independent multiple flares.