  Non-blazar radio-galaxies emitting in the very-high-energy (VHE; >100 GeV)
regime offer a unique perspective for probing particle acceleration and
emission processes in black hole (BH) accretion-jet systems. The misaligned
nature of these sources indicates the presence of an emission component that
could be of hadronic origin and located in the core region. Here we consider
turbulent magnetic reconnection in the BH accretion flow of radio-galaxies as a
potential mechanism for cosmic-ray (CR) acceleration and VHE emission. To
investigate if this scenario is able to account for the observed VHE data, we
combine three numerical techniques to self-consistently model the accretion
flow environment and the propagation of CRs plus electromagnetic cascades
within the accretion flow zone. Here we apply our approach to the radio-galaxy
Centaurus A and find that injection of CRs consistent with magnetic
reconnection power partially reproduce the VHE data, provided that the
accretion flow makes no substantial contribution to the radio-GeV components.
The associated neutrino emission peaks at $\sim10^{16}$ eV and is two orders of
magnitude below the minimum IceCube flux.
