Extreme particle acceleration in magnetic reconnection layers. Application to the gamma-ray flares in the Crab Nebula

TL;DR

This paper proposes a magnetic reconnection model that accelerates particles to PeV energies, explaining the Crab Nebula's gamma-ray flares with a focused electron population producing high-energy synchrotron emission.

Contribution

It introduces a numerical test-particle approach in reconnection layers, demonstrating how particles reach extreme energies and produce observed gamma-ray spectra in the Crab Nebula.

Findings

Particles are accelerated to PeV energies within reconnection layers.

The model reproduces the gamma-ray spectrum peaking above 100 MeV.

Inverse Compton emission is negligible, matching observations.

Abstract

The gamma-ray space telescopes AGILE and Fermi detected short and bright synchrotron gamma-ray flares at photon energies above 100 MeV in the Crab Nebula. This discovery suggests that electron-positron pairs in the nebula are accelerated to PeV energies in a milliGauss magnetic field, which is difficult to explain with classical models of particle acceleration and pulsar wind nebulae. We investigate whether particle acceleration in a magnetic reconnection layer can account for the puzzling properties of the flares. We numerically integrate relativistic test-particle orbits in the vicinity of the layer, including the radiation reaction force, and using analytical expressions for the large-scale electromagnetic fields. As they get accelerated by the reconnection electric field, the particles are focused deep inside the current layer where the magnetic field is small. The electrons suffer less from synchrotron losses and are accelerated to extremely high energies. Population studies show that, at the end of the layer, the particle distribution piles up at the maximum energy given by the electric potential drop and is focused into a thin fan beam. Applying this model to the Crab Nebula, we find that the emerging synchrotron emission spectrum peaks above 100 MeV and is close to the spectral shape of a single electron. The flare inverse Compton emission is negligible and no detectable emission is expected at other wavelengths. This mechanism provides a plausible explanation for the gamma-ray flares in the Crab Nebula and could be at work in other astrophysical objects such as relativistic jets in active galactic nuclei.