Modeling individual nearby radio galaxies as ultra-high-energy cosmic-ray accelerators

Nearby radio galaxies are among the most promising candidates for the acceleration of ultra-high-energy cosmic rays (UHECRs). In this work, we develop a physically motivated, source-resolved framework to quantify the contribution of the three nearest Fanaroff–Riley Class I (FR-I) radio galaxies – Centaurus A, Virgo A, and Fornax A – to the UHECR flux measured by the Pierre Auger Observatory. Acceleration spectra derived from detailed jet-acceleration models are combined with numerical simulations of extragalactic propagation, while the more distant radio-galaxy population is treated as a continuous background. By fitting our simulation exclusively to the measured UHECR energy spectrum, we determine the relative contribution of each source and constrain the fraction of jet power converted into UHECR luminosity. We find that a small number of nearby radio galaxies can account for the highest-energy UHECR flux with acceleration efficiencies of order 10⁻³ 10 - 3 – 10⁻² 10 - 2 , while the background contribution remains subdominant. Some resulting scenarios yield mass-composition trends broadly consistent with observations at the highest energies and predict distinct levels of secondary neutrino fluxes. These results demonstrate that physically grounded, source-specific modeling of nearby radio galaxies provides a physically motivated contribution to the interpretation of the highest-energy UHECR component.