Speaker
Description
Non-jetted AGN exhibit hard X-ray emission with a power law spectrum above $\sim$2 keV, which is thought to be produced through Comptonization of soft photons by electrons and positrons (pairs) in the vicinity of the black hole. The origin and composition of this plasma source, known as the corona, is a matter open for debate.
Our study focuses on the role of relativistic protons accelerated in black-hole magnetospheric current sheets in the pair enrichment and neutrino production of AGN coronae. We present a model that has two free parametears, namely the proton plasma magnetization $\sigma_{\rm p}$, which controls the peak energy of the neutrino spectrum, and the Eddington ratio $\lambda_{\rm Edd}$ (defined as the ratio between X-ray luminosity $L_{\rm X}$ and Eddington luminosity $L_{\rm Edd}$), which controls the amount of energy transferred to secondary particles.
Our results indicate a strong dependence of the neutrino luminosity produced on the Eddington ratio. More specifically, the fraction of the X-ray energy transferred to the high-energy neutrinos produced in the coronal environment is proportional to the Eddington ratio for $\lambda_{\rm Edd} \leq 10^{-2} (\sigma_{\rm p}/10^5)^{-1}$ while constant otherwise. Furthermore, we discuss our results in light of the recent IceCube observations of TeV neutrinos from NGC 1068, NGC 4151 and CGCG 420-015. We, also, combine our coronal model with a luminosity function in order to provide an estimation of the diffuse neutrino flux measured on Earth.
