Self-Consistent Modelling of Neutrino Production in Turbulent Black Hole Coronae

TL;DR

This paper introduces Turb-AM3, a hybrid numerical code for self-consistent modeling of neutrino production in turbulent black hole coronae, successfully reproducing IceCube observations and predicting spectral shapes for future studies.

Contribution

The paper presents a novel hybrid code coupling turbulence-driven particle acceleration with radiative processes, enabling detailed modeling of multi-messenger signals in astrophysical plasmas.

Findings

Reproduces IceCube neutrino signals from NGC 1068 with standard parameters.

Accounts for IceCube observations of other active galactic nuclei.

Predicts spectral shapes for TeV neutrino emissions to guide future observations.

Abstract

Stochastic particle acceleration in magnetized turbulent plasmas has emerged as a key mechanism to explain multi-messenger signals from compact astrophysical environments. Self-consistent modelling remains challenging because it requires to treat simultaneously several non-linear kinetic processes, especially turbulence-driven acceleration and its feedback on the turbulent cascade, as well as the radiative and hadronic losses, including the reprocessing of electromagnetic radiation in radiatively dense environments. The present paper introduces the hybrid numerical code Turb-AM3 designed to this effect. This hybrid numerical code couples the state-of-the-art time-dependent lepto-hadronic radiative solver AM3 with a stochastic acceleration module that incorporates recent theoretical advances in turbulent acceleration and accounts for the dynamical damping of turbulence by accelerated particles. In a second part, we use this code to provide self-consistent time-dependent models of proton acceleration in the turbulent black hole corona of NGC~1068. We find that the IceCube neutrino signal is well reproduced for a standard set of physical parameters describing the black hole corona. The same template model accounts in a satisfactory way for IceCube observations of other active galactic nuclei. Furthermore, our exploration of parameter space allows us to predict detailed template spectral shapes for the TeV neutrino spectrum, which in turn help understand how future neutrino observations can constrain the properties of turbulent AGN coronae and the underlying acceleration mechanism. This Turb-AM3 framework provides a powerful tool to model multi-messenger emission in a broad variety of compact astrophysical environments.