Polarization effects in cosmic-ray acceleration by cyclotron autoresonance

TL;DR

This paper generalizes the theory of cosmic-ray acceleration by cyclotron autoresonance to include any polarization state, demonstrating that certain nuclides can reach ZeV energies in extreme astrophysical conditions with superintense radiation and strong magnetic fields.

Contribution

It introduces a rigorous analytical extension of the cyclotron autoresonance model to arbitrary polarization states and explores its implications for cosmic-ray acceleration.

Findings

Nuclides can reach ZeV energies in astrophysical environments.

Superintense radiation and strong magnetic fields enable acceleration.

The model applies to various wavelengths and intensities.

Abstract

Employing a two-parameter model for representing the radiation field, the theory of cosmic-ray acceleration by cyclotron autoresonance is analytically generalized here to include any state of polarization. The equations are derived rigorously and used to investigate the dynamics of the nuclides $_1$H$^1$, $_2$He$^4$, $_{26}$Fe$^{56}$, and $_{28}$Ni$^{62}$, in severe astrophysical conditions. Single-particle calculations and many-particle simulations show that these nuclides can reach ZeV energies ($1 ~ZeV = 10^{21}$ eV) due to interaction with superintense radiation of wavelengths $\lambda=1~$ and $10~ \mu$m, and $\lambda=50$ pm, and magnetic fields of strengths at the mega- and gigatesla levels. Examples employing radiation intensities in the range $10^{32}-10^{42}$ W/m$^2$ are discussed.