A 3D Diffusive and Advective Model of Electron Transport Applied to the Pulsar Wind Nebula HESS J1825-137

Abstract

HESS J1825-137 is one of the most powerful and luminous TeV gamma-ray pulsar wind nebulae (PWNe), making it an excellent laboratory to study particle transportation around pulsars. We present a model of the (diffusive and advective) transport and radiative losses of electrons from the pulsar PSRJ1826-1334 powering HESSJ1825-137 using interstellar medium gas (ISM) data, soft photon fields and a spatially varying magnetic field. We find that for the characteristic age of 21 kyr, PSR J1826-1334 is unable to meet the energy requirements to match the observed X-ray and gamma-ray emission. An older age of 40 kyr, together with an electron conversion efficiency of 0.14 and advective flow of $v=0.002c$, can reproduce the observed multi-wavelengh emission towards HESS J1825-137. A turbulent ISM with magnetic field of $B=20\mu G$ to $60\mu G$ to the north of HESS J1825-137 (as suggested by ISM observations) is required to prevent significant gamma-ray contamination towards the northern TeV source HESS J1826-130.

Accepted to be published by the Monthly Notices of the Royal Astronomical Society

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Cited by in corpus (1)

• Particle acceleration to PeV energies in Pulsar Wind Nebula: a two zone model