Ultra-high-energy cosmic ray acceleration by magnetic reconnection in relativistic jets and the origin of very high energy emission

TL;DR

This paper demonstrates through 3D relativistic MHD simulations that magnetic reconnection in relativistic jets can efficiently accelerate cosmic rays up to ultra-high energies, explaining observed high-energy emissions in blazars.

Contribution

The study provides the first direct simulation-based evidence that magnetic reconnection in relativistic jets can accelerate particles to ultra-high energies, with detailed analysis of acceleration rates and spectra.

Findings

Particles reach energies up to 10^{20} eV in strong magnetic fields.

Acceleration rate shows weak dependence on particle energy, r_{acc} ∝ E^{-0.1}.

Particle spectra develop a hard power-law tail with index p ∼ -1.2.

Abstract

Relativistic jets are believed to be born magnetically dominated. Very and ultra-high energy cosmic rays can be efficiently accelerated by magnetic reconnection in these sources. We here demonstrate this directly, with no extrapolations to large scales, by means of three-dimensional relativistic magnetohydrodynamical (3D-RMHD) simulations of a Poyinting flux dominated jet. We inject thousands of low-energy protons in the region of a relativistic jet that corresponds to the transition from magnetically to kinetically dominated, where its magnetization parameter is $\sigma \sim 1$. In this region, there is efficient fast magnetic reconnection which is naturally driven by current-driven-kink instability (CDKI) turbulence in the helical magnetic fields of the jet. We find that the particles are accelerated by Fermi process in the reconnection regions (and by drift in the final stages) up to energies $E \sim 10^{18}$ eV for background magnetic fields $B \sim 0.1$ G, and $E \sim 10^{20}$ eV for $B \sim 10$ G. We have also derived from the simulations the acceleration rate due to magnetic reconnection which has a weak dependence on the particles energy $ r_{acc} \propto E^{-0.1}$, characteristic of exponential growth. The energy spectrum of the accelerated particles develops a power-law tail with spectral index $p \sim -1.2$. This hardness of the spectrum must decrease when particle losses and feedback into the background plasma are included. Our results can explain observed flux variability in the emission of blazars at the very high energy band as well as the associated neutrino emission. Successful applications of our results to the blazars MRK 421 and TXS 0506+056 are also discussed.