# Hyper-Resistive Model of Ultra High Energy Cosmic Ray Acceleration by Magnetically Collimated Jets Created by Active Galactic Nuclei

## TL;DR

This paper presents a hyper-resistive MHD model linking dynamo processes in AGN accretion disks to the formation of magnetically collimated jets, explaining their role in accelerating ultra high energy cosmic rays beyond 10^19 eV.

## Contribution

It introduces a novel hyper-resistive MHD framework that connects dynamo formation to large-scale jet collimation and cosmic ray acceleration, bridging simulations and observations.

## Key findings

- Model predicts jet length, opening angle, and power consistent with observations.
- Explains how jets accelerate particles to ultra high energies (>10^19 eV).
- Provides nine observable predictions matching astrophysical data.

## Abstract

This is the fourth in a series of companion papers showing that, when an efficient dynamo can be maintained by accretion disks around supermassive black holes in Active Galactic Nuclei (AGNs), it will lead to the formation of a powerful, magnetically-collimated helix that could explain both the observed jet/radiolobe structures on very large scales and ultimately the enormous power inferred from the observed ultra high energy cosmic rays (UHECRs) with energies > 10^19 eV. Many timescales are involved in this process. Our hyper-resistive magnetohydrodynamic (MHD) model provides a bridge between General Relativistic MHD simulations of dynamo formation, on the short accretion timescale, and observational evidence of magnetic collimation of large-scale jets on astrophysical timescales. Given the final magnetic structure, we apply hyper-resistive kinetic theory to show how instability causes slowly-evolving magnetically-collimated jets to become the most powerful relativistic accelerators in the Universe. The model yields nine observables in reasonable agreement with observations: the jet length, radiolobe radius and apparent opening angle as observed by synchrotron radiation; the synchrotron total power, synchrotron wavelengths and maximum electron energy (TeVs); and the maximum UHECR energy, the cosmic ray energy spectrum and the cosmic ray intensity on Earth.