Flares in the Crab Nebula Driven by Untwisting Magnetic Fields

TL;DR

This paper proposes a model where untwisting magnetic fields around the Crab pulsar accelerate particles rapidly via localized resistivity, explaining observed gamma-ray flares and PeV electrons within a day.

Contribution

It introduces a novel acceleration mechanism involving untwisting magnetic fields and localized resistivity, accounting for rapid gamma-ray flares and ultra-high-energy electrons in the Crab nebula.

Findings

Reproduces flare time scales of about 1 day

Matches observed peak photon energies around 1 MeV

Explains electron energies reaching 1 PeV

Abstract

The recent discovery of PeV electrons from the Crab nebula, produced on rapid time scales of one day or less with a sharply peaked gamma-ray spectrum without hard X-rays, challenges traditional models of diffusive shock acceleration followed by synchrotron radiation. Here we outline an accleration model involving a DC electric field parallel to the magnetic field in a twisted toroidal field around the pulsar. Sudden developments of resistivity in localized regions of the twisted field are thought to drive the particle acceleration, up to PeV energies, resulting in flares. This model can reproduce the observed time scales of $T \approx 1$ day, the peak photon energies of $U_{\Phi,rr} \approx 1$ MeV, maximum electron energies of $U_{e,rr} \approx 1$ PeV, and luminosities of $L \approx 10^{36}$ erg s$^{-1}$.