  Magnetic field-aligned electric fields are characteristic features of
magnetic reconnection processes operating in externally agitated magnetized
plasmas. An especially interesting environment for such a process are the
coronae of accretion disks in active galactic nuclei (AGN). There, Keplerian
shear flows perturb the quite strong disk magnetic field leading to intense
current sheets. It was previously shown that given field strengths of 200 G in
a shear flow, reconnection driven magnetic field aligned electric fields can
accelerate electrons up to Lorentz factors of about 2000 in those objects thus
providing us with a possible solution of the injection (pre-acceleration)
problem. However, whereas in the framework of magnetohydrodynamics the
formation of the field-aligned electric fields can be described consistently,
the question has to be addressed whether the charged particles can really be
accelerated up to the maximum energy supplied by the field-aligned electric
potentials, since the accelerated particles undergo energy losses either by
synchrotron or inverse Compton mechanisms. We present relativistic particle
simulations starting from electric and magnetic fields obtained from
magnetohydrodynamic simulations of magnetic reconnection in an idealized AGN
configuration including nonthermal radiative losses. The numerical results
prove that the relativistic electrons can be effectively accelerated even in
the presence of an intense radiation bath. Energies from 50 MeV up to 40 GeV
can be reached easily, depending on the energy density of the photon bath.
