# Numerical models of neutrino and gamma-ray emission from magnetic reconnection in the core of radio-galaxies

## TL;DR

This paper models neutrino and gamma-ray emissions from magnetic reconnection in radio-galaxies' cores, suggesting a partial explanation for VHE data and predicting neutrino fluxes below IceCube detection levels.

## Contribution

It introduces a combined numerical approach to simulate particle acceleration and emission in the accretion flow of radio-galaxies, specifically applying it to Centaurus A.

## Key findings

- CR injection can partially reproduce VHE data
- Neutrino emission peaks at ~10^16 eV
- Neutrino flux is two orders below IceCube limits

## Abstract

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.