  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.
