  In the present paper we investigate the production of ultrahigh energy cosmic
rays (UHECRs) from Seyferts. We discuss the UHECR luminosities obtained by two
possible engine trigger models: pure radiative transfer and the energy
extraction from poloidal magnetic flux. The first case is modeled by Kerr slim
disk or Bondi accretion mechanisms. Since it is assumed that the broadband
spectra of Seyferts indicate that at least the outer portions of their
accretion disks are cold and geometrically thin, and since our results point
that the consequent radiative energy transfer is inefficient, we build the
second approach based on massive Seyferts with sufficient central poloidal
magnetic field to trigger an outflow of magnetically driven charged particles
capable to explain the observed UHECRs and gamma rays in Earth experiments from
a given Seyfert source.
