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

TL;DR

This study models nearby radio galaxies as sources of ultra-high-energy cosmic rays, using detailed acceleration and propagation models to explain observed UHECR flux and composition.

Contribution

It introduces a source-resolved framework combining jet-acceleration models with propagation simulations to quantify individual radio galaxy contributions to UHECRs.

Findings

Nearby radio galaxies can explain the highest-energy UHECR flux.

Acceleration efficiencies are of order 10^{-3} to 10^{-2}.

Predicted secondary neutrino fluxes are consistent with observations.

Abstract

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 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 exclusively 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 $10^{-3}-10^{-2}$, while the background contribution remains subdominant. The resulting scenarios yield mass-composition trends broadly consistent with observations and predict distinct levels of secondary neutrino fluxes. These results demonstrate that physically grounded, source-specific modeling of nearby radio galaxies provides a viable and predictive explanation for the origin of the highest-energy cosmic rays.