Numerical models of neutrino and gamma-ray emission from magnetic reconnection in the core of radio-galaxies
J.C. Rodriguez-Ramirez*, E.M. de Gouveia Dal Pino and R. Alves Batista
Full text: pdf
Pre-published on: May 13, 2019
Published on: May 21, 2019
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.
DOI: https://doi.org/10.22323/1.329.0014
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