The shape of Fe K$\alpha$ line emitted from relativistic accretion disc
  around AGN black holes
  The relativistically broadened Fe K$\alpha$ line, originating from the
accretion disc in a vicinity of a super massive black hole, is observed in only
less than 50\% of type 1 Active Galactic Nuclei (AGN). In this study we
investigate could this lack of detections be explained by the effects of
certain parameters of the accretion disc and black hole, such as the
inclination, the inner and outer radius of disc and emissivity index. In order
to determine how these parameters affect the Fe K $\alpha$ line shape, we
simulated about 60,000 Fe K $\alpha$ line profiles emitted from the
relativistic disc.
  Based on simulated line profiles, we conclude that the lack of the Fe
K$\alpha$ line detection in type 1 AGN could, be caused by the specific
emitting disc parameters, but also by the limits in the spectral resolution and
sensitivity of the X-ray detectors.
