Magnetically Heated Coronae above Accretion Disks

Fraction of energy generated in the hot corona above accretion disk in active galactic nuclei (AGN) can be self consistently determined when heating of corona by magnetic field reconnection is assumed. Nevertheless, the quantitative estimations of properties of the corona depend on the model of cool accretion disk below. We present how the detailed, non averadged vertical structure of an accretion disk influences the principal parameters of the corona.